adsabs/AstroCLIMB huggingface dataset:
Paper: Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy
Authors: I. Martinez-Castellanos, Leo P. Singer, E. Burns, D. Tak, Alyson Joens, Judith L. Racusin, Jeremy S. Perkins
Figure caption: Simple multiresolution map. A single base pixel is highlighted (compare with Figure 1). A cylindrical projection of (c) is shown in Figure 4.
Paper: Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy
Authors: I. Martinez-Castellanos, Leo P. Singer, E. Burns, D. Tak, Alyson Joens, Judith L. Racusin, Jeremy S. Perkins
Figure caption: This figure exemplifies how pixels are automatically split during arithmetic operations depending on whether the user defines a map as density-like (b) or histogram-like (c). We use integers for simplicity, however both density-like and histogram-like maps can contain floating point values.
Paper: Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy
Authors: I. Martinez-Castellanos, Leo P. Singer, E. Burns, D. Tak, Alyson Joens, Judith L. Racusin, Jeremy S. Perkins
Figure caption: (a) Numbering of base HEALPix pixels (NSIDE = 1). (b), (c) Pixel numbers for a map with NSIDE = 2 under the RING and NESTED schemes, respectively. A single base pixel is highlighted.
Paper: Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy
Authors: I. Martinez-Castellanos, Leo P. Singer, E. Burns, D. Tak, Alyson Joens, Judith L. Racusin, Jeremy S. Perkins
Figure caption: (a) GW170817 sky localization probability density map by LIGO and Virgo (Abbott et al. 2017) (b) Corresponding probability map integrated on the mesh resulting from an adaptive refinement process.
Paper: Multiresolution HEALPix Maps for Multiwavelength and Multimessenger Astronomy
Authors: I. Martinez-Castellanos, Leo P. Singer, E. Burns, D. Tak, Alyson Joens, Judith L. Racusin, Jeremy S. Perkins
Figure caption: Pixelization of the sphere for various NSIDE values. The center of the pixels, along isolatitude lines, are represented with dots. A single base pixel is highlighted.
Paper: Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk’s H2O Ice Line
Authors: Henrique Reggiani, Kevin C. Schlaufman, Brian F. Healy, Joshua D. Lothringer, David K. Sing
Figure caption: 1D non-LTE carbon and oxygen abundances of WASP-77 A compared to the same 1D non-LTE abundances for solar neighborhood dwarfs from GALAH DR3 (Buder et al. 2021). In each kernel density estimator-smoothed scatter plot, darker blue regions correspond to more densely populated regions of abundance space. We plot outliers as individual dots. We plot our abundance inferences for WASP-77 A's as black-bordered white points. Left: [C/H], [C/Fe], [O/H], and [O/Fe]. Right: [(C + O)/H], [(C + O)/Fe], [C/O], and C/O. In the range −0.1 ≤ [Fe/H] ≤ 0, WASP-77 A is consistent with the GALAH-inferred carbon (﹩[{\rm{C}}/\mathrm{Fe}]={0.05}_{-0.10}^{+0.12}﹩), oxygen (﹩[{\rm{O}}/\mathrm{Fe}]={0.06}_{-0.10}^{+0.14}﹩), and C/O abundance ratio distributions (﹩[{\rm{C}}/{\rm{O}}]={0.01}_{-0.12}^{+0.11}﹩ and ﹩{\rm{C}}/{\rm{O}}={0.49}_{-0.12}^{+0.15}﹩). In the metallicity range −0.5 ≤ [Fe/H] ≤ 0.5 appropriate for virtually all known exoplanet host stars, GALAH DR3 finds that 95% of solar neighborhood dwarf stars have −0.15 ≤ [C/Fe] ≤ 0.32, −0.19 ≤ [O/Fe] ≤ 0.43, −0.26 ≤ [C/O] ≤ 0.29, and 0.27 ≤ C/O ≤ 0.94. These broad distributions emphasize that the assumption of solar abundance ratios of carbon and oxygen for exoplanet host stars is not always appropriate.
Paper: Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk’s H2O Ice Line
Authors: Henrique Reggiani, Kevin C. Schlaufman, Brian F. Healy, Joshua D. Lothringer, David K. Sing
Figure caption:  RadVel fit of a Keplerian orbit to the WASP-77 A differential radial velocities from Maxted et al. (2013), as updated in Trifonov et al. (2020). We fix the orbital period P = 1.3600306 ± 0.0000012 to the value from Turner et al. (2016) and the eccentricity to zero as expected for short-period hot Jupiter orbiting a mature solar-type star. Using the stellar mass we inferred from our self-consistent analysis of astrometric, photometric, and spectroscopic data for WASP-77 A M * = 0.92 ± 0.02 M ⊙ we find that WASP-77 A b’s mass is M p = 1.66 ± 0.03 M Jup.
Paper: Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk’s H2O Ice Line
Authors: Henrique Reggiani, Kevin C. Schlaufman, Brian F. Healy, Joshua D. Lothringer, David K. Sing
Figure caption: Samples from photospheric and fundamental stellar parameter posteriors from our Bayesian analyses of astrometric, photometric, and spectroscopic data for WASP-77 A. We emphasize that our adopted [Fe/H] comes from averaging individual equivalent width-based iron abundance inferences as described above and not directly from the isochrones-inferred metallicity plotted here.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Best-fit Keplerian orbital model for the WASP-4 system for Models #1 (top left), #2 (top right), #3 (bottom left), and #4 (bottom right) using RadVel. (a) panels: the maximum-likelihood model is plotted while the orbital parameters listed in Table 4 are the median values of the posterior distributions. The thin blue line is the best-fit model. We add in quadrature the RV jitter terms listed in Table 4 with the measurement uncertainties for all RVs. (b) panels: residuals to the best-fit model. The error bars of the residuals reflect both the measurement error and the jitter from the MCMC fit. The larger error bars for the one-planet fits reflect the larger amounts of jitter needed to fit the data with only one planet. (c) panels: RVs phase-folded to the ephemeris of WASP-4b. The phase-folded model for WASP-4b is shown as the blue line. The Keplerian orbital models for all other planets (if modeled) have been subtracted. (d) panels: RVs phase-folded to the ephemeris of the second planet, WASP-4c. The Keplerian orbital model for the other planet (panels (c), WASP-4b) has been subtracted. Red circles are the velocities binned in 0.08 units of orbital phase.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Forward models of the TTV signal of WASP-4b produced by the possible outer companion. These models were created using OCFit. The models used the priors as listed in Table 4, where the outer planet has an eccentricity of 0.094 (Model #4). The two objects are assumed to be coplanar.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: TESS light curve of WASP-4b in Sectors 2, 28, and 29. Top: raw simple-aperture photometry light curves. Bottom: detrended DVT.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: WASP-4b transit (panels (a), (b), and (c)) and occultation (panel (d)) timing variations after subtracting the data with a constant-period model. The filled black triangles are the data points from the literature and the square orange points are from the TESS data in this paper. All the transit and occultation times can be found in Table 5. The orbital decay and apsidal precession models are shown as the blue and red lines, respectively.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Phase-folded transit light curve of WASP-4b from TESS. The unbinned and binned data are shown in blue and black, respectively. The binned transit has been binned by 5 minutes. The best-fitting model obtained from EXOMOP is shown as a solid red line. The residuals (light curve – model) are shown below the light curve.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Phased-folded occulation PDC light curve of WASP-4b from TESS. The unbinned and data binned by 18 minutes are shown in black and red, respectively. The vertical dashed lines show the time range of the expected secondary eclipse.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Comparison of detrending results between the eleanor and unpopular packages. In the top panel, we show the two detrended light curves. Similar to Feinstein et al. (2019), we remove the three transit signals (purple shaded regions) and three specific periods (gray shaded regions) before calculating the 1 hr CDPP using the lightkurve package. The first region is when an asteroid crossed the aperture, the second region is when an improper spacecraft configuration caused high pointing jitter, and the third region is when scattered light from the Moon caused large spikes. The unpopular light curve has a lower 1 hr CDPP of 356 ppm. To obtain the unpopular light curve, we chose a 3 × 3 aperture centered on the source, did not add a polynomial component, performed the initial background subtraction, and set L = 256, λ  L  = 0.01, k = 150. In the bottom panels, we show the detrended light curves around the three transit signals. The transit depths are comparable between the two light curves.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Analysis of Sector 11 TIC 39513064 data. In the top panel, we show the background-subtracted and normalized FFI data (black), the systematics prediction/model from the unpopular package (red), and the detrended light curve (blue) centered around zero. The two dips at the beginning of each orbit are due to the initial background subtraction overcorrecting the scattered-light signal. In the middle panel, we show the SPOC 2 minute light curve binned to 30 minutes (orange) and the detrended unpopular FFI light curve (blue). Two regions of strong scattered light at the beginning of each orbit were removed in the SPOC light curve, as it affected the SPOC pipeline’s systematics removal process. In the bottom left panel, we plot the Lomb–Scargle periodograms for these two light curves, showing that they both peak at 0.413 day. We folded both light curves with this period and show them in the bottom right panel. To obtain the unpopular light curve, we used the SPOC aperture, performed an initial background subtraction, did not add a polynomial component, and set L = 256, λ  L  = 1, k = 150.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Different detrending results for the central pixel of ASASSN-18tb when varying λ  L  and λ  P  while fixing L = 256, k = 126. Each panel shows the detrended pixel light curve and 6 hr CDPP for a specific combination of λ  L  and λ  P . The value of λ  L  increases from the left column to the right column, and the value of λ  P  increases from the top row to the bottom row. The smallest 6 hr CDPP values of ∼904 ppm are obtained in the top four rows of the third column, where λ  L  = 10−2 and λ  P  = 0, 10−3, 10−2, and 10−1. The bottom left panels show signs of the systematic component overfitting to the long-term trend, while the right columns show signs of underfitting
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Detrended pixel light curves (top panel) and detrended aperture light curve (bottom panel). Each of the light curves in the top panel are the detrended versions of those shown in Figure 5. The aperture light curve is obtained by first scaling each pixel light curve to its estimated physical flux and then summing them together. No initial background subtraction was performed, a cubic polynomial was added to capture the long-term trend, and we set L = 256, λ  L  = 0.01, λ  P  = 0.01, and k = 126.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Different detrending results for the central pixel of ASASSN-18tb when varying k, the number of sections to use for the train-and-test framework. Other tuning parameters were kept constant (L = 256, λ  L  = λ  P  = 10−2). Each section is indicated by contiguous points of the same color (noncontiguous points of the same color are different sections). As k becomes larger, the 6 hr CDPP decreases, while the runtime increases. While most values of k show similar results, when k = 2, the systematic effects around 1348–1350 days are still present in the detrended light curve.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Difference between the choice of predictor pixels based on the selection method. In both panels, the pixel being detrended is the central pixel (blue star). The exclusion region around the central pixel (shaded and hatched orange area) is where predictor pixels are not chosen from. In the left panel, the predictor pixels (red circles) were chosen based on having a similar median brightness to the pixel being detrended. In the right panel, the predictor pixels were chosen based on having a high cosine similarity to the pixel being detrended. The clustering of predictor pixels in the right panel indicates that there are local systematic effects in this region.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Multisector detrended light curve of the TDE ASASSN-19bt. Each sector was detrended separately, and the detrended light curves were stitched together as described in the text. For each sector, we chose a 3 × 3 aperture centered on the source, did not perform an initial background subtraction, added a cubic polynomial, and set L = 256, λ  L  = λ  P  = 0.01, k = 150.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: The 6 hr CDPP and runtime for detrending the central pixel of ASSASSN-18tb as a function of k (L = 256, λ  L  = λ  P  = 10−2). Note that the x-axis is scaled logarithmically. The 6 hr CDPP fluctuates while decreasing until around k ∼ 45 and then shows a significant decrease beyond that point. It then shows marginal decreases from k ∼ 100, while the runtime increases roughly linearly.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: Some properties of the systems containing newly validated planets. Top: the new host stars (large circles with black edges) compared to the host stars of known planets at the NASA Exoplanet Archive. Bottom: the new planets (large circles with black edges) compared to the planets with measured radii and orbital periods shorter than 100 days at the NASA Exoplanet Archive. K2-399 b is highlighted, which is an ultra-hot, Saturn-sized planet in a relatively unpopulated region of parameter space.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: Transmission spectroscopy values (top) and emission spectroscopy values (bottom) for the newly validated planets (small points) and planets slated for observation in JWST Cycle 1 (large points), color-coded by their equilibrium temperature. In each case the shaded regions indicate areas of interest as identified by Kempton et al. (2018).
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: The metallicity distribution of the host stars of planets with measured radii (3411 planets at the NASA Exoplanet Archive). The green, blue, and purple contours enclose 68%, 95%, and 99.7% of the data, respectively. K2-408 b has one of the lowest well-constrained metallicities measured to date for an exoplanet host star.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: Centroid plots for candidates with significant (p-value < 0.05) centroid offsets during transit. The contours show the 1σ, 2σ, and 3σ contours for the centroid locations for out-of-transit cadences; the gray points show the remaining out-of-transit centroid locations that fall outside those contours. The blue points are the centroid locations of the in-transit cadences.
Paper: Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18
Authors: Jessie L. Christiansen, Sakhee Bhure, Jon K. Zink, Kevin K. Hardegree-Ullman, Britt Duffy Adkins, Christina Hedges, Timothy D. Morton, Allyson Bieryla, David R. Ciardi, William D. Cochran, Courtney D. Dressing, Mark E. Everett, Howard Isaacson, John H. Livingston, Carl Ziegler, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, David W. Latham, Michael Endl, Phillip J. MacQueen, Benjamin J. Fulton, Lea A. Hirsch, Andrew W. Howard, Lauren M. Weiss, Bridgette E. Allen, Arthur Berberyann, Krys N. Ciardi, Ava Dunlavy, Sofia H. Glassford, Fei Dai, Teruyuki Hirano, Motohide Tamura, Charles Beichman, Erica J. Gonzales, Joshua E. Schlieder, Thomas Barclay, Ian J. M. Crossfield, Emily A. Gilbert, Elisabeth C. Matthews, Steven Giacalone, Erik A. Petigura
Figure caption: A portion of the light curve of EPIC 205957328, showing two transits of the short-period candidate EPIC 205957328.01, and a potential single transit of a longer-period candidate centered at ∼2211 days.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Depletion of NH3 in the center of H-MM1. Left: KDE comparison between NH3 and H2 column densities. This presents a positive correlation below N(H2) < 2.6 × 1022 cm−2, whereas for higher N(H2) values the NH3 column density is nearly constant or decreasing to a small degree. The black horizontal segments show the mean values within the N(H2) bins. The red line shows a broken straight line fit to the data (see text). Right: map of the fractional NH3 abundance, X(NH3) = [NH3]/[H2], calculated as the ratio between the column densities. The NH3 abundance drops significantly in the central region, and the distribution is asymmetric so that ammonia is more abundant on the western side of the core as compared to the eastern side. The contours show the H2 column density starting at 1 × 1022 cm−2 and with a spacing of 1 × 1022 cm−2. The beam size and scale bar are shown as in Figure 1.