adsabs/AstroCLIMB huggingface dataset:
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Left: the best-fitting mass between 200 and 300 pc (red circles), and within the half-mass radius (black empty squares) vs. the truth. The black dashed line marks y = x to guide the eye. Right: the best-fitting mass between 200 and 300 pc (red circles) and within the half-mass radius (black empty squares) vs. the specific star formation rate (sSFR). The black dashed line marks y = 0 to guide the eye. In both plots, the best fits are achieved using the double power-law model profile for the underlying dark matter, with free inner slopes, while the M/L, is fixed to the true value of unity. Only bound star particles are used as tracers, and no observational errors are included for results in this plot. Red circles with a green star symbol represent star-forming systems with prominent galactic winds. Red circles with a blue diamond represent systems with a larger than zero SFR but without obvious galactic winds. Red circles with a cyan square represent nearby Sagittarius-like dwarfs undergoing tidal strippings. A sample of 6000 star particles is used for the dynamical constraint of each system, and the statistical uncertainties are smaller than or comparable to the symbol size.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: The ﹩x^{\prime} ﹩ component of the mean velocity (left) and velocity dispersion (right) profiles of star particles, binned along the major (green) and minor (black) axes for Au16-9. Note that along the major and minor axes, only stars within sectors of ±45° to the corresponding axes are used to calculate the mean velocity and velocity dispersion in each bin. Each bin contains 100 stars. The x and y errors indicate the bin width and the 1σ scatters, respectively. Green and black solid curves denote the model predictions along the major and minor axes, based on the NFW model profile. Blue and magenta solid curves denote the model predictions along the major and minor axes, based on the double power-law model profile for the dark matter with free inner slopes. Dashed curves around the solid ones with corresponding colors indicate the 1σ uncertainties in the model. The green, black, blue, and magenta curves in the left panel are all very close to the horizontal lines at y = 0, and hence are overlapping each other.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Red circles denote besting-fitting vs. true masses between 200 and 300 pc. This is similar to the left plot of Figure 2, but we use a smaller tracer sample of 2000 bound star particles, and only use their line-of-sight velocities after including observational errors (foreground/background contamination is not modeled). After excluding systems with less than 2000 bright stars (see Section 2.2 for details), only 16 systems are left. The meanings of the filled symbols with different colors and shapes are the same as those in Figure 2. Black empty triangles are repeats of the corresponding red empty circles in Figure 2. Errors for back empty triangles are similar to or smaller than the symbol size, and thus are not shown.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: The likelihood contours of all possible combinations of every two out of the five model parameters for Au16-9 (NFW potential model with free M/L and 6000 star particles as tracers). The yellow contour includes 10% of the MCMC sample centered on the best fits. The light blue and two dark blue contours represent the 1σ, 2σ, and 3σ confidence levels. The degeneracies between the tracer parameters (κ and b) and the potential parameters (M/L, ﹩{d}_{1}={\mathrm{log}}_{10}{\rho }_{s}^{2}{r}_{s}^{3}﹩, and ﹩{d}_{2}={\mathrm{log}}_{10}{\rho }_{s}﹩) are very weak, but there are stronger degeneracies among M/L, d 1, and d 2.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Differences between the proper motions after incorporating realistic observation errors and the true proper motions, reported as a function of the CSST g-band apparent magnitudes. We only show the ﹩x^{\prime} ﹩ component, as the ﹩y^{\prime} ﹩ component is very similar. Black (left) and red (right) points denote foreground/background stars and member stars of Au16-9 in the simulation, respectively. The proper motion errors are for either Gaia DR3 (top panels) or for CSST (bottom panels). The dense clumps at g ∼ 18.4 in the right panels correspond to the red giant branch bump. Gaia DR3 proper motion errors are about a factor of 2 smaller than the upper limits in CSST errors at 18 < g < 19.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Similar to Figure 4, but shows the true (green dots) and best-fitting (magenta curves) total mass profiles for four representative star-forming systems with outflows. Black vertical lines mark the half-mass radii.
Paper: Is the Core-cusp Problem a Matter of Perspective? Jeans Anisotropic Modeling against Numerical Simulations
Authors: Wenting Wang, Ling Zhu, Zhaozhou Li, Yang Chen, Jiaxin Han, Feihong He, Xiaohu Yang, Yipeng Jing, Carlos Frenk, Jialu Nie, Hao Tian, Chao Liu, Yanan Cao, Xiaoqing Qiu, John Helly, Robert J. J. Grand, Facundo A. Gomez
Figure caption: Similar to Figure 6, this figure shows the ﹩x^{\prime} ﹩ component of the mean velocity (left) and velocity dispersion (right) profiles, of star particles binned along the major (green) and minor (black) axes for Au21-9.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Pre-explosion mass distribution for the LSNe, SLSNe, SNe Ic, and SNe Ic-BL populations, normalized by their respective sample sizes. We estimate the progenitor mass by summing the best-fit value of the ejecta mass with the mass of the remnant neutron star. SLSNe have a sharp drop-off at the low-mass end, where SNe Ic peak, and LSNe are intermediate between these two populations. The same trend is seen in the high-mass end: SLSNe extend to very high masses of ∼40 M ⊙, LSNe appear to max out at ∼30 M ⊙, and SNe Ic/Ic-BL have almost no objects above ∼20 M ⊙. Dashed lines are linear fits to the distributions above 10 M ⊙ and below the N = 1 SN threshold. The peak in the LSNe distribution at ∼2 M ⊙ is driven entirely by two objects with tightly constrained M ej values (iPTF16asu and SN 2021lwz).
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Left: fractional contribution of the magnetar component to the total output luminosity of the light curve (magnetar plus radioactive decay) for all the SNe in our sample as a function of days since explosion. Right: posterior model distribution for the same fractional magnetar contribution, but integrated over the first 200 days of the SN. We include 150 samples for each SN and normalize the populations by their respective sample sizes. SLSNe appear magnetar dominated and mostly remain as such throughout their evolution, whereas SNe Ic are mostly radioactively dominated. While some LSNe appear magnetar dominated, some seem to be powered entirely by radioactive decay.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Best-fit nickel mass as a function of ejecta mass for the LSNe, SLSNe, SNe Ic, and SNe Ic-BL populations. For clarity, we exclude the SLSNe with unconstrained nickel mass fractions (i.e., those for which even f Ni = 0.5 still provides a subdominant contribution to the light curve). The dashed lines indicate f Ni = 0.01, 0.1, 1. LSNe mostly occupy a similar range to SNe Ic/Ic-BL, but also overlap the parameter space occupied by SLSNe. The higher luminosities of LSNe compared to SNe Ic/Ic-BL indicates an additional contribution from magnetar engines.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Best-fit magnetar spin period and magnetic field values for the LSNe, SLSNe, SNe Ic, and SNe Ic-BL populations. The upper left corner, where most SLSNe lie, is dominated by powerful fast-spinning magnetars, whereas in the bottom right corner, populated by SNe Ic/Ic-BL, the magnetar power is low and the observed optical emission is dominated by radioactive decay. Some LSNe appear powered by magnetars similar to those in SLSNe, some have intermediate power magnetars, and some have weak or no magnetar contribution.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Best-fit MOSFiT parameters for the SLSNe, SNe Ic, SNe Ic-BL, and LSNe populations. The green circles represent the Gold LSNe sample, while the diamonds represent the Silver sample. Other SNe types are shown as faded circles for comparison. We see that SLSNe and SNe Ic/Ic-BL separate very well in terms of most parameters, while LSNe span almost the entire range of allowable models, further emphasizing their intermediate nature.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Light curves and spectra of the Slow SLSN-like LSNe group. Only r-band light curves and their respective MOSFiT models are shown. Spectra are arbitrarily scaled. Individual references are listed in Appendix A.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Ejecta mass as a function of rise time for the LSNe, SLSNe, SNe Ic, and SNe Ic-BL population. We see that, like previously established for SLSNe (e.g., Nicholl et al. 2015; Könyves-Tóth & Vinkó, 2021) and SNe Ic/Ic-BL (e.g., Dessart et al. 2016), LSNe with longer rise times tend to have larger ejecta masses.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Rise time as a function of peak r-band absolute magnitude for the LSNe, SLSNe, SNe Ic, and SNe Ic-BL populations. We find that, by definition, LSNe occupy a very clear space in terms of peak magnitude, but they also have intermediate rise times between those of SLSNe and SNe Ic/Ic-BL.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Light curves and spectra for the Fast SLSN-like LSNe group. Only r-band light curves and their respective MOSFiT models are shown. Spectra are arbitrarily scaled. Individual references are listed in Appendix A.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Virtual spacecraft data for the CME1–CME2 interaction with a waiting time of 20 hr between their respective launches. This corresponded to a merger of the CME sheaths at approximately 0.9 au. The time series in solid blue, dotted yellow, and dashed green lines refer to the signatures of CME1–CME2, CME1, and CME2, respectively.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Virtual spacecraft time series data at 1 au of CME1 shown in Figure 3. CME1 has a tilt angle τ = 180° and handedness H = +1. Further parameters for CME1 are specified in Table 1. The blue shaded region indicates the region of the shock and sheath and the yellow shaded region the ejecta/flux rope.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: CME1 Spheromak simulation with initial tilt angle τ = 180° and handedness H = +1, 30 hr after launch. (a) Shows the normalized density, (b) the radial velocity, and (c) (B GSE) z  in the equatorial plane. Further CME1 parameters are specified in Table 1.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Meridional plane profiles and selected magnetic field lines for the collision of CME1 and CME2, 40 hr after CME1 initialization. Each handedness variation is shown (a) and (b) for a waiting time of 20 hr and tilt angles of τ = 180°.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: CME1–CME2 interaction with a waiting time of 20 hr between their launches. (a) shows the normalized density, (b) the radial velocity, and (c) the (B GSE) z  in the equatorial plane.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Magnetic field time series at 1 au for CME1 for different initial tilt angles.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Maximal values for the range of tilt angles CME1 is simulated for. (a) shows v  r , (b) shows the density, ρ  r , (c) the dynamic pressure, P ram, (d) ﹩{({B}_{\mathrm{GSE}})}_{z}﹩, (e) the predicted Dst, and (f) the predicted subsolar magnetopause standoff distance, R mp.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Maximal values for the range of waiting times CME1 and CME2 are simulated for. (a) shows v  r , (b) shows the density, ρ  r , (c) the dynamic pressure, P ram, (d) ﹩{({B}_{\mathrm{GSE}})}_{z}﹩, (e) the predicted Dst, and (f) the predicted subsolar magnetopause standoff distance, R mp.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Virtual spacecraft data for the CME1–CME2 interaction with a waiting time of 28 hr between their respective launches. This corresponded to the merger of the CME flux ropes at approximately 0.9 au. The time series in solid blue, dotted yellow, and dashed green lines refer to the signatures of CME1–CME2, CME1, and CME2, respectively.
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Comparison of Cassini de Thury’s sunspot drawing during the partial solar eclipse of 1727 September 15 (HARS 1727, p. 397) with our calculation of the heliographic coordinates and lunar shade during the greatest magnitude of this partial eclipse, as observed from Paris Observatory. Note that we interpreted Cassini de Thury’s drawing as a mirrored image. Here, the abbreviations read as follows: N (the celestial north), Z (the zenith), P (the position angle of the northern extremity of the axis of rotation of the Sun measured eastward from N), L 0 (the heliographic longitude of the solar center), B 0 (the heliographic latitude of the solar center), and V (the position angle of the northern extremity of the axis of the Sun measured counterclockwise from Z).
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Comparison of sunspot positions in 1727–1748 derived in the present study (black circles) and from previous studies: Wargentin (blue diamonds; A18) and Staudach (green diamonds; Arlt 2009).
Paper: An Overview of Sunspot Observations in 1727–1748
Authors: Hisashi Hayakawa, Kentaro Hattori, Mitsuru Sôma, Tomoya Iju, Bruno P. Besser, Shunsuke Kosaka
Figure caption: Comparison of Weidler’s sunspot drawing during the Mercury transit of 1736 November 11 (Weidler 1739) with our calculation of the heliographic coordinates and path of the Mercury transit, as observed from Wittenberg. Note that we interpreted Weidler’s drawing as an erect image, correcting the annotation of Weidler’s N–S orientation.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: The black histograms are the HCO+ spectra at the positions shown with black crosses in Figure 1, which are separated by 49″ in both R.A. and decl.. The panel with the blue asterisk represents the spectrum at the millimeter dust peak. The red histograms show the corresponding C18O (2–1) spectra. The spectra of both molecules are normalized to their peak values, which are indicated in the top-left corner of each panel (in K, first for HCO+, and then for C18O). The vertical dotted line (in red) shows the centroid velocity obtained by fitting a single Gaussian profile to the C18O data. The same figure in absolute flux units is reported in Appendix A.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Input quantities and radiative transfer results for the initial model with no added envelope. Top panel: the solid black curve shows the HCO+ abundance profile predicted by the chemical model at t = 106 yr and with an external visual extinction A V = 5 mag, compared with the H2 volume density profile taken from the physical model (dashed green curve; both quantities are shown in logarithmic scale). Middle panel: comparison between the gas kinetic temperature of the model (dashed red curve) and the excitation temperature profile of the (1–0) transition computed by MOLLIE (solid blue line). Bottom panel: the observed HCO+ (1–0) spectra toward the L1544 dust peak (black histogram) compared with the synthetic spectrum computed with MOLLIE using the abundance profile shown in the top panel (red histogram).
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Top panel: the solid curves show the original physical model computed by Keto et al. (2015): H2 volume density profile (green curve), gas temperature profile (red curve), and dust temperature profile (blue curve). The dashed extensions of the curve represent the properties of the isothermal, uniform envelope described in 4.2.1 that extends from r = 0.32 pc (shown with the vertical black line) to 1.0 pc. Bottom panel: same as the top, but for the velocity profile, shown in orange.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Panel (a): excitation temperature profiles of the HCO+ (1–0) transition obtained with the model with the extended, static envelope, at three different volume densities: n env = 133 cm−3 (blue curve), n env = 53 cm−3 (green curve), and n env = 27 cm−3 (red curve). Panels (b) to (d): synthetic spectra obtained with the radiative transfer for the corresponding models presented in panel (a). The observed spectrum is shown with the black histogram and gray shadow in each panel.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Top panel: the green curve shows the CO abundance profile predicted by the chemical model at t = 106 yr and with an external visual extinction A V = 5 mag, extended in the 1 pc envelope. The blue curve shows the excitation temperature profile of the (1–0) transition computed by MOLLIE. Bottom panel: the observed CO (1–0) spectra toward the L1544 dust peak (black histogram) compared with the synthetic spectra computed with MOLLIE using the abundance profile shown in the top panel (red histogram). The observed spectra are from A. Chacón-Tanarro et al. (2022, in preparation).
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Left panel: comparison between the HCO+ (1–0) spectrum (black histogram) and the ortho-H2O(11,0 − 10,1) (blue curve) spectrum observed by Herschel/HIFI (Caselli et al. 2012), taken at the millimeter dust peak of L1544. The water line has been scaled up by a factor of 80 to allow for an easier comparison. Right panel: same as in the left panel, but this time the blue histogram shows the isolated hyperfine component ﹩F{{\prime} }_{{\rm{N}}}\to {F}_{{\rm{N}}}=0\to 1﹩ of the ortho-NH3(10 − 00) line (from Caselli et al. 2017), and it has been scaled by a factor of 15. All the spectra have been smoothed to the same resolution of 40″. Note the spectral resolution of the HIFI instrument at the frequencies of the H2O and NH3 lines is ≈ 0.065 km s−1, hence comparable to that of the HCO+ data. Both panels are shown with the same y-axis range.