adsabs/AstroCLIMB huggingface dataset:
Paper: Cosmology with Binary Neutron Stars: Does Mass–Redshift Correlation Matter?
Authors: Soumendra Kishore Roy, Lieke A. C. van Son, Anarya Ray, Will M. Farr
Figure caption: Injection-recovery results for the fiducial model (top) and the I. Mandel & B. Müller (2020) remnant mass and natal kick prescription (bottom). Left: kernel density estimates of the m1 – z and m2 – z populations from COMPAS simulations. In both models, peaks and dips remain stationary with redshift, changing only in absolute merger rate based on star formation, suggesting that the BNS mass function is roughly redshift-independent. Right: inferred matter density and Hubble constant values for both correlated (blue) and uncorrelated (green) populations. Our framework accurately recovers cosmological parameters using both evolving and nonevolving mass models based on mock data from 800 BNSs (about 6 days of xG observations at the median BNS merger rate; R. Abbott et al. 2023a). For both the fiducial and I. Mandel & B. Müller (2020) models, we achieve ∼2% constraints on the Hubble constant, comparable to N. Aghanim et al. (2020) and A. G. Riess et al. (2022), and therefore sufficient to address the Hubble tension.
Paper: Cosmology with Binary Neutron Stars: Does Mass–Redshift Correlation Matter?
Authors: Soumendra Kishore Roy, Lieke A. C. van Son, Anarya Ray, Will M. Farr
Figure caption: The posterior distribution of the Hubble constant for different numbers of detected BNSs. Left: the evolving (blue) and nonevolving (green) mass models are consistent with each other up to approximately 3000 BNS observations, which corresponds to one month of data. We achieve percent-level precision in the Hubble constant within this time frame when we fix the population. For larger numbers of BNS observations, the width of the posterior does not change significantly, indicating that it is suppressed by ﹩1/\sqrt{N}﹩, where N is the number of BNS observations. Right: the inferred redshift evolution of the Hubble parameter, H(z), divided by (1 + z). H(z) is best constrained near z = 0.4, achieving a less than 0.5% error bar. We accurately recover the true curve when we fix the population to the nonevolving mass model. The forecasted error bars from the DESI Collaboration et al. (2016) are also overlaid.
Paper: Cosmology with Binary Neutron Stars: Does Mass–Redshift Correlation Matter?
Authors: Soumendra Kishore Roy, Lieke A. C. van Son, Anarya Ray, Will M. Farr
Figure caption: The corner plots show the COMPAS populations of masses and redshifts for both the fiducial setup and the Mandel–Müller kick prescription for the remnant mass, along with the GMM fit of these populations. In the upper left plot of the fiducial population, fewer than 10 events following a northwest-to-southeast path (﹩\mathrm{log}q\approx -0.7﹩ to −0.5) are not captured by the GMM. However, since the chirp mass of these events still falls within the GMM-covered population—and chirp mass is the most precisely measured parameter in cosmological PE—there is no resulting bias in the cosmological parameters.
Paper: Cosmology with Binary Neutron Stars: Does Mass–Redshift Correlation Matter?
Authors: Soumendra Kishore Roy, Lieke A. C. van Son, Anarya Ray, Will M. Farr
Figure caption: The corner plots and histograms display the marginalized distributions of masses and redshifts for both the fiducial and Mandel–Müller populations, along with their GMM fits. Code to generate these plots is available at https://github.com/SoumendraRoy/RedevolBNS/blob/main/Make_Plots/Appendix_Plots.ipynb.
Paper: Cosmology with Binary Neutron Stars: Does Mass–Redshift Correlation Matter?
Authors: Soumendra Kishore Roy, Lieke A. C. van Son, Anarya Ray, Will M. Farr
Figure caption: Comparison of individual NS mass measurements with the BNS mass population from the fiducial setup in COMPAS. Left: mass measurements from Gaia and NICER are overlaid on the fiducial mass spectrum. Here the y-axis is scaled arbitrarily. Right: PE contours for GW170817 and GW190425 are shown against the fiducial population.
Paper: The Striated Solar Photosphere Observed at ﹩0\mathop{.}\limits^{^{\prime\prime} }03﹩ Resolution
Authors: David Kuridze, Friedrich Wöger, Han Uitenbroek, Matthias Rempel, Alexandra Tritschler, Thomas Rimmele, Catherine Fischer, Oskar Steiner
Figure caption: Overview of the MURaM simulation of a plage-like atmosphere. Top row: vertical magnetic flux density and vertical velocity at the horizontally averaged height where the optical depth τ500 nm is unity. Middle row: synthetic G-band images at disk center (μ = 1, left panel) and off disk center (μ = 0.85, right panel) computed from the MURaM snapshot using the RH code. The limb direction is downward and the y-axis is foreshortened for the limbward image in the right panel. Bottom panel: synthetic G-band spectrum (blue line) at disk center averaged over the full FOV. The orange line represents the FTS atlas profile from H. Neckel & D. Labs (1984) for comparison, while the green line depicts the experimental transmission profile of the VBI G-band filter.
Paper: The Striated Solar Photosphere Observed at ﹩0\mathop{.}\limits^{^{\prime\prime} }03﹩ Resolution
Authors: David Kuridze, Friedrich Wöger, Han Uitenbroek, Matthias Rempel, Alexandra Tritschler, Thomas Rimmele, Catherine Fischer, Oskar Steiner
Figure caption: Top: synthetic G-band image of a simulation snapshot (left panel) and corresponding map of the height where the optical depth reaches unity in the G-band continuum at 430.7 nm. The red contour indicates the location of a dark lane starting at x, y ≈ (0, 2.4) in the G-band image. The limb is in the downward direction of the images. Bottom: vertical cuts through the temperature and LoS magnetic field strength along the blue dotted line marked in the top panels. Isothermal contours at T = 6000 and 7000 K are overplotted as white lines. Blue lines follow the τ = 1 height.
Paper: The Striated Solar Photosphere Observed at ﹩0\mathop{.}\limits^{^{\prime\prime} }03﹩ Resolution
Authors: David Kuridze, Friedrich Wöger, Han Uitenbroek, Matthias Rempel, Alexandra Tritschler, Thomas Rimmele, Catherine Fischer, Oskar Steiner
Figure caption: G-band intensity profiles along the crosscuts of dark/bright striae marked with red dashes in the top-left observed G-band image. Gaussian fits of the individual profiles are overplotted in red.
Paper: First Detection of Low-frequency Striae in Interplanetary Type III Radio Bursts
Authors: Vratislav Krupar, Eduard P. Kontar, Jan Soucek, Lynn B. Wilson, Adam Szabo, Oksana Kruparova, Hamish A. S. Reid, Mychajlo Hajos, David Pisa, Ondrej Santolik, Milan Maksimovic, Jolene S. Pickett
Figure caption: Zoomed-in view of the type III striae detected by Cluster’s WBD. (a) Spectral profiles at 17:39:32 UT and 17:49:35 UT in the 52–60 kHz range, each exhibiting four identifiable striae peaks. (b) Gaussian fits to the peaks, used to derive the parameters in Table 1. The colored lines correspond to individual striae.
Paper: The Striated Solar Photosphere Observed at ﹩0\mathop{.}\limits^{^{\prime\prime} }03﹩ Resolution
Authors: David Kuridze, Friedrich Wöger, Han Uitenbroek, Matthias Rempel, Alexandra Tritschler, Thomas Rimmele, Catherine Fischer, Oskar Steiner
Figure caption: Left: zoomed image of the G-band facular region indicated by the white box in Figure 1. Right: the same image processed with a Gaussian-filter subtraction method (see text for an explanation). The direction arrow points in the direction of the DC.
Paper: First Detection of Low-frequency Striae in Interplanetary Type III Radio Bursts
Authors: Vratislav Krupar, Eduard P. Kontar, Jan Soucek, Lynn B. Wilson, Adam Szabo, Oksana Kruparova, Hamish A. S. Reid, Mychajlo Hajos, David Pisa, Ondrej Santolik, Milan Maksimovic, Jolene S. Pickett
Figure caption: Comparison of striae parameters at low and high frequencies by I. N. Sharykin et al. (2018). (a) Bandwidth Δf, (b) Drift rate −df/dt, and (c) Relative density fluctuations Δn/n, each plotted vs. observing frequency. Simple power-law fits (dashed lines) are shown for reference.
Paper: The Striated Solar Photosphere Observed at ﹩0\mathop{.}\limits^{^{\prime\prime} }03﹩ Resolution
Authors: David Kuridze, Friedrich Wöger, Han Uitenbroek, Matthias Rempel, Alexandra Tritschler, Thomas Rimmele, Catherine Fischer, Oskar Steiner
Figure caption: Mosaic of high-resolution G-band filtergrams obtained with the VBI instrument on 2022 June 3 at 17:46 UT. The white box indicates the plage region shown in Figure 2.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Left panel: equatorial distributions of the out-of-equilibrium chemical potentials ﹩{\mu }_{{\rm{\Delta }}}^{npl}﹩ (left portions) and ﹩{\mu }_{{\rm{\Delta }}}^{npl\nu }﹩ (right portions) for lepton flavors l = e, μ in the 5-ν scenario at ﹩\bar{t}=7.0\,{\rm{ms}}﹩, i.e., when ﹩{\langle {\mu }_{{\rm{\Delta }}}^{npl\nu }\rangle }_{{\rm{xy}}}\simeq 0﹩. The dotted, dashed–dotted, dashed, and solid lines show rest-mass density contours at 1011, 1012, 1013, and 1014 g cm−3, respectively. Right panel: the same as in the left panel but at ﹩\bar{t}=27.9\,{\rm{ms}}﹩ and on the (x, z)-plane. For compactness, we show distributions for npe (left portions) and npeν (right portions) equilibria but contrast the 5-ν (upper part) with the 3-ν (bottom part) scenario. Note that ﹩{\mu }_{{\bar{\nu }}_{\mu }}\gt {\mu }_{{\bar{\nu }}_{e}}﹩ in the 5-ν case (left panel) and that ﹩{\mu }_{{\bar{\nu }}_{e}}﹩ is reduced in the 5-ν case (right panel) because of the considerable differences in ﹩{\mu }_{{\bar{\nu }}_{e}}﹩ in the high-density regions.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Top panel: evolution of the maximum rest-mass density ﹩{\rho }_{{\rm{\max }}}﹩, maximum temperature ﹩{T}_{{\rm{\max }}}﹩, and mass-averaged temperature 〈T〉xy on the (x, y)-plane for the 5-ν (solid lines) and 3-ν (dashed lines) scenarios. Bottom panel: neutrino luminosities (total and species-specific) ﹩{{ \mathcal L }}_{\nu }﹩ at 300 km; the data are smoothed using time averaging over 0.2 ms. In both panels, the shaded region denotes the time when ﹩{\mu }_{{\rm{\Delta }}}^{npe\nu }\approx {\mu }_{{\rm{\Delta }}}^{np\mu \nu }\approx 0﹩ (see gray shaded regions in Figure 8 in Appendix A for the SFHo and DD2 EOSs).
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Distributions of the proton fraction Yp at ﹩\bar{t}=1.9\,{\rm{ms}}﹩ (left column), 7.8 ms (middle column), and 19.3 ms (right column). The top (bottom) row shows the polar (equatorial) distributions, and for each panel, the right (left) portions refer to the 5-ν (3-ν) scenarios, respectively. Note the differences that develop and the significantly lower protonization at late times when accounting for five neutrino species.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Distributions of the normalized ejected mass for the 5-ν (solid lines) and 3-ν (dashed lines) scenarios as functions (from left to right) of the proton fraction Yp, the polar angle θ, the temperature T, and the terminal velocity v∞. The data are extracted on a two-sphere detector at 300 km. Shown with red lines are the total distributions, while green and blue lines refer respectively to ﹩\bar{t}\leqslant 4.0\,{\rm{ms}}﹩ and ﹩\bar{t}\geqslant 4.0\,{\rm{ms}}﹩ (different times reflect the different speeds of the ejecta to reach the detector). In all cases, Yp ≈ Ye, since Yμ ≲ 5 × 10−3.
Paper: Accurate Muonic Interactions in Neutron Star Mergers and Impact on Heavy-element Nucleosynthesis
Authors: Harry Ho-Yin Ng, Carlo Musolino, Samuel D. Tootle, Luciano Rezzolla
Figure caption: Comparison between the solar relative abundances (black filled circles) as a function of the mass number A and the nucleosynthetic yields from the 5-ν (red line) and 3-ν (blue line) scenarios; both abundances are rescaled to match at A = 132. Note the better match with data for lanthanides 139 < A < 176 (blue shaded region) and for very heavy elements with 190 < A < 215 (orange shaded region); very light elements with 70 < A < 110 (gray shaded region) are significantly suppressed.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: Expanded view of emission around the wavelength of the H2 17 μm S(1) line from the Peak region of the Taurus molecular cloud integrated over the area of the mosaicked observation. Only a linear baseline has been removed. Note that for a resolving power R equivalent to a velocity resolution of 120 km s−1 the observed spectrum is essentially the response of the MIRI spectrometer rather than being the emission-line profile.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: The two regions observed in the H2 S(1) transition in the boundary of the Taurus molecular cloud overlaid on an image of the 13CO J = 1→0 integrated intensity (adapted from P. F. Goldsmith et al. 2008). The sizes of the regions, denoted “Edge” and “Peak,” have been significantly expanded to make them visible.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: Distribution of intensity from off-line (“background”) channels (green) and summed on-line (“line”) channels (blue) for the Edge (left) and Peak (right) regions in the Taurus molecular cloud boundary.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: H2 S(1) emission from the Peak region of the Taurus molecular cloud. The contours are at levels of 30 and 36 MJy sr−1.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: H2 S(1) emission from the Edge region of the Taurus molecular cloud. The contours are at a level of 20 MJy sr−1.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: Output covering essentially the entire spectral range of JWST/MIRI Channel 3–Long from the Peak region of the Taurus molecular cloud integrated over the area of the mosaicked observation. Only a linear baseline has been removed. The H2 S(1) emission is the only strong line that is visible.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: Top panel: dependence of the quantity n(3)A3,1 characterizing the emission from the J = 3 level of ortho-H2 on total H2 density and kinetic temperature. The five blue curves are labeled by their kinetic temperature. The horizontal dashed cyan line shows log(n(3)A3,1) = −7.44, corresponding to an observed intensity of 10 MJy sr−1. The intersection of this line with the curve for given kinetic temperature (here 1000 K) determines the total H2 density (here ≃350 cm−3), as indicated by the vertical dotted–dashed cyan line. Bottom panel: excitation temperature of the S(1) line as a function of total H2 density and kinetic temperature. The vertical solid cyan line indicates the excitation temperature, 800 K, determined by the selected kinetic temperature and the derived H2 density.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: Total H2 density as a function of kinetic temperature for the given J = 3 column density, N(J = 3). The three curves are for the column density corresponding to intensity 10 MJy sr−1 and factor of 3 greater and smaller column density than this.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: Relative integration times for pixels in the 4 × 4 mosaic of pointings of the subband C, Channel 3 MIRI/MRS array used for observations of the 17.04 μm S(1) line in the Taurus boundary regions.
Paper: The H2 Glow of a Quiescent Molecular Cloud Observed with JWST
Authors: Paul F. Goldsmith, Shengzhe Wang, Xin Wang, Raphael Skalidis, Gary A. Fuller, Di Li, Chao-Wei Tsai, Lile Wang, Donghui Quan
Figure caption: 12CO and 13CO J = 1 → 0 spectra from the survey carried out with the 14 m FCRAO antenna (P. F. Goldsmith et al. 2008). Top panel: in the region encompassing the Peak position. Bottom panel: the same lines for the region encompassing the Edge position. The vertical cyan lines identify the velocity of the strongest 13CO emission at each position.
Paper: A Coherent Radio Burst from an X-Ray Neutron Star in the Carina Nebula
Authors: K. M. Rajwade, J. Tian, G. Younes, B. Posselt, B. Stappers, Z. Wadiasingh, E. D. Barr, M. C. Bezuidenhout, M. Caleb, F. Jankowski, M. Kramer, I. Pastor-Marazuela, M. Surnis
Figure caption: Radio burst from 2XMM J104608.7−594306 showing linear polarization (red), circular polarization (blue), and the polarization position angle (black points). The pulse has been coherently dedispersed at the DM that maximizes the S/N. The bottom panel shows a dynamic spectrum of the total intensity as a function of time and observing frequency, with horizontal excisions for RFI.
Paper: A Coherent Radio Burst from an X-Ray Neutron Star in the Carina Nebula
Authors: K. M. Rajwade, J. Tian, G. Younes, B. Posselt, B. Stappers, Z. Wadiasingh, E. D. Barr, M. C. Bezuidenhout, M. Caleb, F. Jankowski, M. Kramer, I. Pastor-Marazuela, M. Surnis
Figure caption: Images of the field of 2XMM J104608.7−594306  integrated over the duration of the radio burst (left) and before the burst detection (center), and the difference between the two images (right). The magenta circle marks the transient source identified at the time of the burst detection, and the inset at the bottom right corner shows a zoomed-in view to display the position (in red) of the XDIN candidate 2XMM J104608.7−594306 on top of the transient source. The images have a synthesized beam size of 43″ × 9″. The black ellipse in the inset at the bottom right corner of the left panel shows the synthesized beam.
Paper: A Coherent Radio Burst from an X-Ray Neutron Star in the Carina Nebula
Authors: K. M. Rajwade, J. Tian, G. Younes, B. Posselt, B. Stappers, Z. Wadiasingh, E. D. Barr, M. C. Bezuidenhout, M. Caleb, F. Jankowski, M. Kramer, I. Pastor-Marazuela, M. Surnis
Figure caption: X-ray vs. radio luminosity for various coherent radio-emitting sources. The shaded region shows the range of X-ray luminosities for XDINSs, CCOs, and 2XMM J104608.7−594306. The dashed gray lines denote constant ratios of the radio and X-ray luminosity (radio luminosity computed at 1.4 GHz). We note that the X-ray fluxes for pulsars, XDINSs, and CCOs are the persistent X-ray fluxes reported in D. L. Kaplan & M. H. van Kerkwijk (2009), I. F. Malov & M. A. Timirkeeva (2018), T. Prinz & W. Becker (2015), F. Haberl (2007), and A. De Luca (2017) for CCOs, while for magnetars, we use values from G. L. Israel et al. (2021), P. Esposito et al. (2020), F. Camilo et al. (2018), and C. D. Bochenek et al. (2020), and the references therein. For pulsar, we use fluxes based on the power-law fit in T. Prinz & W. Becker (2015) in the 0.1–2 KeV band and extrapolate them to 0.2–10 keV. The radio luminosities for pulsars and magnetars are the period-averaged radio luminosities (R. N. Manchester et al. 2005), i.e., based on the continuum radio flux at 1.4 GHz. Here, radio pseudoluminosity refers to the product of the average radio flux density and the square of the distance, while the radio luminosity is calculated by multiplying the pseudoluminosity by 4π (to denote isotropic radio luminosity). The values for SGR J1935+2154 are taken from C. D. Bochenek et al. (2020) and F. Kirsten et al. (2021).
Paper: A Coherent Radio Burst from an X-Ray Neutron Star in the Carina Nebula
Authors: K. M. Rajwade, J. Tian, G. Younes, B. Posselt, B. Stappers, Z. Wadiasingh, E. D. Barr, M. C. Bezuidenhout, M. Caleb, F. Jankowski, M. Kramer, I. Pastor-Marazuela, M. Surnis
Figure caption: Schematic of a phenomenological model of the observed radio emission from 2XMM J104608.7−594306. Different active zones spawned at varied times and altitudes near a magnetic pole arrive at an observer from higher altitudes and more oblique angles at later times. This can explain the observed frequency evolution of emission and the flattening of the PPAs. The left panel denotes the emission seen at time t1 while the right panel is the emission seen at time t2 > t1 (observer frame).
Paper: First Detections of PN, PO, and PO+ toward a Shocked Low-mass Starless Core
Authors: Samantha Scibelli, Andrés Megías, Izaskun Jiménez-Serra, Yancy Shirley, Jennifer Bergner, Judit Ferrer Asensio, Robin T. Garrod, Mélisse Bonfand, Anissa Pokorny-Yadav
Figure caption: Dust temperature (color scale) and N(H2) column density (contours: 1, 2, 3, 4, 5, 6, 7, and 8 × 1022 cm−2) Herschel maps of NGC 1333 region in Perseus (S. Pezzuto et al. 2021). Included are the locations of four starless and prestellar cores, Pers264, Pers317, Pers321, and Pers326 (black circles 38″ in size) and the locations of the prominent CO outflows in the region, SVS 13A, IRAS 4A, and IRAS 2A, as described in A. L. Plunkett et al. 2013. (Note: the length of jet arrows are not to scale).
Paper: First Detections of PN, PO, and PO+ toward a Shocked Low-mass Starless Core
Authors: Samantha Scibelli, Andrés Megías, Izaskun Jiménez-Serra, Yancy Shirley, Jennifer Bergner, Judit Ferrer Asensio, Robin T. Garrod, Mélisse Bonfand, Anissa Pokorny-Yadav
Figure caption: SiO(1–0) emission observed toward Pers326 with the Yebes 40 m telescope (black) and a Gaussian fit to the line (blue). The vertical dashed lines correspond to the vlsr of 7.6 km s−1. Additional SiO emission toward the other nearby starless cores Pers321 (orange), Pers317 (red), and Pers264 (gray) are also plotted for reference.
Paper: First Detections of PN, PO, and PO+ toward a Shocked Low-mass Starless Core
Authors: Samantha Scibelli, Andrés Megías, Izaskun Jiménez-Serra, Yancy Shirley, Jennifer Bergner, Judit Ferrer Asensio, Robin T. Garrod, Mélisse Bonfand, Anissa Pokorny-Yadav
Figure caption: PO+ transitions observed toward Pers326. In solid red is the Gaussian fit to the detected (>3σ) line, and the dotted lines are LTE fits at Tex = 4.6 K. The vertical dashed line shows the consistent vlsr of 7.6 km s−1, and the horizontal gray line shows the 1σ noise level. Spectra are offset by 40 mK for easier viewing.