adsabs/AstroCLIMB huggingface dataset:
Paper: Pitch-angle Anisotropy Imprinted by Relativistic Magnetic Reconnection
Authors: Luca Comisso, Brian Jiang
Figure caption: Snapshots of the electric current density and the mean kinetic energy per particle in the statistical steady-state regime for magnetic reconnection with varying guide-field strength. The top-to-bottom panels correspond to guide-field strengths of (a) B  g  = B 0/8, (b) B  g  = B 0, and (c) B  g  = 8B 0 for the out-of-plane current density J  z  (in units of en 0 c), while panels (d), (e), and (f) illustrate the cell-averaged mean kinetic energy per particle 〈γ − 1〉cell (normalized by m  e  c 2) for the same guide-field strengths. The snapshots are taken at times around ﹩t\sim 2{L}_{x}{({B}_{0}^{2}+{B}_{g}^{2})}^{1/2}/{B}_{0}c﹩, corresponding to similar stages of nonlinear evolution. To emphasize the small-scale structures in the reconnection layer, we limit the displayed domain region to ∣y∣ ≤ 150d  e .
Paper: Pitch-angle Anisotropy Imprinted by Relativistic Magnetic Reconnection
Authors: Luca Comisso, Brian Jiang
Figure caption: Mean of the squared pitch angle sine, ﹩\langle {\sin }^{2}\alpha \rangle ﹩, at late times, ﹩t\simeq 3{L}_{x}{({B}_{0}^{2}+{B}_{g}^{2})}^{1/2}/{B}_{0}c﹩, for simulations with (a) fixed σ 0 = 16 and varying guide-field strengths B  g  = (1/8, 1/4, 1/2, 1, 2, 4, 8)B 0 and (b) fixed B  g /B 0 = 1 and varying lepton magnetization σ 0 = (4, 8, 16, 32, 64). Horizontal dashed black lines indicate the expectation for isotropic particles, ﹩\langle {\sin }^{2}\alpha \rangle =2/3﹩. In addition, dashed lines indicating power-law slopes are provided for reference.
Paper: Pitch-angle Anisotropy Imprinted by Relativistic Magnetic Reconnection
Authors: Luca Comisso, Brian Jiang
Figure caption: Particle energy spectra ﹩{dN}/d\gamma ﹩ at late times, ﹩t\,\simeq 3{L}_{x}{({B}_{0}^{2}+{B}_{g}^{2})}^{1/2}/{B}_{0}c﹩, when the spectra have fully developed. Panel (a) showcases simulations with fixed σ 0 = 16 and varying guide-field strengths B  g  = (1/8, 1/4, 1/2, 1, 2, 4, 8)B 0, while panel (b) features simulations with fixed B  g /B 0 = 1 and varying lepton magnetization σ 0 = (4, 8, 16, 32, 64). Dashed lines indicating power-law slopes are provided for reference.
Paper: Pitch-angle Anisotropy Imprinted by Relativistic Magnetic Reconnection
Authors: Luca Comisso, Brian Jiang
Figure caption: 2D histograms illustrating the power-law indices p < (panel (a)) and p > (panel (b)), characterizing the nonthermal tail of the particle energy spectrum produced by magnetic reconnection, as a function of the dimensionless guide-field strength B  g /B 0 and the magnetization σ 0.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: The absolute B-band magnitude of CCSN host galaxies as a function of redshift. Our hosts are found in the least luminous (10−3 L ⋆) to the most luminous star-forming galaxies (≲5L ⋆) (L ⋆ is the characteristic luminosity of the B-band luminosity function of star-forming galaxies). Most Ca-rich IIb hosts have luminosities of 10−2 to a few L ⋆, similar to regular CCSNe (indicated by the contours encircling 68%, 90%, and 95% of the PTF+iPTF CCSN sample; Schulze et al. 2021). We also indicate the L ⋆ presented in Faber et al. (2007) and multiples of it in gray.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: The measured O mass lower limits are shown with the horizontal dashed lines. The O yields for the ejecta arising from the He-star progenitor models, which assume an evolution in a binary system (Dessart et al. 2021), are shown with filled blue circles, and those arising from the single-star models (Sukhbold et al. 2016) are shown with filled orange stars. We also plot the O mass for nucleosynthetic models of higher-ZAMS stars (Nomoto et al. 1997; Rauscher et al. 2002; Limongi & Chieffi 2003) and for lower-ZAMS stars from USSN models of Yoshida et al. (2017) and Moriya et al. (2017).
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: The red plus signs show the [O I] luminosities calculated from the nebular spectra for the Ca-rich Type IIb sample. The luminosity is normalized to the 56Co decay energy. We compare these to models of stripped-envelope CCSNe from Jerkstrand et al. (2015). We also show the measured normalized [O I] luminosities from the nucleosynthesis calculations of Yoshida et al. (2017) and the Ca-rich Type IIb iPTF 15eqv.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Comparison of the ejecta properties we observe (horizontal dashed lines) for our sample with that for the explosion models based on He stars evolved with the nominal mass-loss rate from Dessart et al. (2021; filled circles). From top to bottom, we show the ejecta mass M ej, ejecta kinetic energy E kin, 56Ni mass, and oxygen yield.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: The host population in the mass−SFR plane. All sources exploded in star-forming galaxies. This is illustrated by their location with respect to the main sequence of star-forming galaxies (gray shaded region). The majority of hosts also have properties consistent with those of CCSNe from the PTF+iPTF surveys (gray contours indicate the region encircling 68%, 90%, and 95% of the sample; Schulze et al. 2021).
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Comparison of the observed explosion energy values with predictions from Burrows et al. (2019; B19) and Burrows & Vartanyan (2021; B22). They use the CCSN code FORNAX to perform 2D and 3D CCSN simulations for a range of progenitor masses. See Section 4.1.2 for details.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: The projected physical offset distribution of all the SNe in our sample compared with the distribution for other types of SNe measured in De et al. (2020). We note that there is a distinct offset from the gap Ca-rich Type I SNe, known to occur in quenched environments.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: The full wavelength range of the nebular spectra shown in Figure 3. The phase of the spectra is measured as the number of rest-frame days since the second peak.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: The g − r color evolution of the SNe in our sample (red plus signs), compared to the Type IIb SN sample of Taddia et al. (2018; gray diamonds).
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: Representative geometric model of the Hβ emission in the BLR of NGC 3227. The left panel is oriented edge-on, with an Earth-based observer at large +x values, and the right panel shows the Earth-based observer's view. The transparency of each point is related to the strength of the response of the gas, with more opaque points having a stronger response to continuum fluctuations.
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: Median velocity-delay map Ψ(λ, τ) created by randomly selecting several Hβ models from the posterior probability distributions. Integrating the velocity-delay map over wavelength (velocity) gives the one-dimensional lag profile Ψ(τ), which is shown on the right. Integrating over time delay gives Ψ(λ), or the variable emission-line profile, which is shown immediately under the map. The bottom panel displays the average lag as a function of wavelength across the emission line, with the turquoise crosses showing the average time delay for five velocity bins across the Hβ profile from Figure 5.
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: Left: Hβ and model light curves, shown as black points and blue curve, respectively. Right: mean and rms line profile in black and gray, respectively, and the model mean and rms line profiles in blue and light blue, respectively, for broad Hβ. The narrow Hβ line profile is in yellow, and the overall fit is in red. The light curve and line profile models were created using BELMAC with parameters interpreted from Table 4.
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: Same as Figure 9, but with model parameters adjusted to best match the Hβ light curve, line profile, and rms profile.
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: Histograms displaying the posterior distributions of the BLR model parameters for Hβ.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Results for three different ST+PST runs: panels (A) and (B) refer to the SE 0.3, ET 0.1, LP 104, MM on, LR run on data generated with the ST+PST model and noise realization 1; panel (C) to the SE 0.3, ET 0.1, LP 6 × 103, MM on, LR run on data generated with the ST+PST model and noise realization 3; and panel (D) to the SE 0.3, ET 0.1, LP 104, MM on, LR run on data generated with the ST-U model and noise realization 1. Mode numbers are specified only for analyses employing the mode-separation modality (also referred to as mode-separation variant). Panel (B) corresponds to the maximum likelihood sample belonging to the secondary mode; all other panels refer to the maximum likelihood sample of their respective inference runs. Top panels: schematic representation of the hot spot configurations, as seen from Earth. Bottom panels: difference in counts between the injected data and the expected counts corresponding to the considered sample of their respective runs (for reference, in the injected data the maximum count per phase bin and channel is ∼700). The small differences in counts, always smaller than ∼twice the Poisson noise standard deviation, imply that significantly different configurations and parameter values can arise from very similar data sets, assuming the current properties of the PSR J0030+0451 NICER observations.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Background figure for the ST+PST inference run SE 0.3, ET 0.1, LP 104, MM on, LR on data created with the same model and noise realization 1. In shades of pink, from the lightest to the darkest, we highlight the contribution to the data in counts per channel of the primary hot spot, the secondary hot spot, and the background. The solid pink and dashed fuchsia lines represent, respectively, the total counts per channel expected according to our model and found in the data. With the solid purple line, we show the background correspondent to the maximum likelihood sample of the inference run. From the strongest to the dimmest purple regions, we show the ±1, ±2, and ±3 standard deviation regions. The solid black and the dashed gray lines (mostly overlapping) show the background added to the hot spot contribution to obtain the simulated data with the ST+PST and ST-U models, respectively.
Paper: Pitch-angle Anisotropy Imprinted by Relativistic Magnetic Reconnection
Authors: Luca Comisso, Brian Jiang
Figure caption: (a) Time evolution of the reconnection rate R rec for simulations with magnetization σ 0 = 16 spanning a broad range of guide-field strengths B  g . (b) Time-averaged reconnection rate (〈R rec〉) and maximum outflow velocity normalized to the speed of light (〈v out〉/c) during the statistical steady-state regime (t ≳ L  x /c after the peak of the reconnection rate) for the same simulations. (c) 2D histogram of the statistical steady-state reconnection rate 〈R rec〉 as a function of the dimensionless guide-field strength B  g /B 0 and the magnetization σ 0.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: Upper panel: Two-color image highlighting the presence of two CO (3–2) velocity components toward the 1.2 mm continuum source N 105–1 A. The CO (3–2) redshifted (241–243 km s−1) and blueshifted (233–235 km s−1) velocity components are shown in red and cyan, respectively. Both the blue and red single contours correspond to 0.17 Jy beam−1 km s−1 and outline the lower emission boundaries of the two velocity components. The 1.2 mm continuum contours are shown in yellow with contour levels of (10, 30, 250)σ (see also Figure 1). The size of the synthesized beam (0.″41 × 0.″33) is indicated in the lower left corner of the image. Lower panel: The CO (3–2) position–velocity diagram along the gray rectangle shown in the image in the upper panel (X–X′). The x-axis shows an offset from the 1.2 mm continuum peak (source 1 A) indicated with the white dotted line; the offset directions are labeled X and X′ to ease a comparison to the image in the upper panel. The horizontal red and cyan dotted lines show the CO (3–2) integrated velocity ranges used to plot the redshifted and blueshifted velocity components in the image in the upper panel.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The left panel shows hydrogen recombination lines observed toward N 105–1 A in Band 6 (from top to bottom in order of decreasing frequency): H36β, H41γ, H53η, H54η, and H49ϵ. The hydrogen recombination lines observed toward N 105–1 A in Band 3 are shown in the right panel (from top to bottom): H40α, H50β, and H57γ. The observed spectra are shown in light gray; the spectra shown in color were smoothed using the Hanning window with the window size of 11 (Band 6) and 5 (Band 3; using PyAstronomy.pyasl.smooth). The dashed and dotted lines in the left panel indicate the central velocity of the H36β (231.9 km s−1) and H13CO+ (237.2 km s−1) lines, respectively, while the dashed line in the right panel indicates the central velocity of the H40α line (230.1 km s−1). The fitted Gauss functions are overlaid. The results of the fitting are reported in Table 1.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: Integrated Hn α (stacked α-transitions; upper panel) and H40α (lower panel) line intensities as a function of bolometric luminosity (L bol) for the Galactic H II regions with the detection of mm-RLs (Kim et al. 2017) with the position of N 105–1 A indicated with the red diamond. The integrated H40α line intensity (not corrected for beam dilution) is plotted for 1 A in both plots. Galactic sources with asymmetric submm-RLs discussed in Kim et al. (2018) are also overlaid as indicated in the legend. The integrated H40α line intensity observed toward 1 A is similar to that observed toward the most luminous Galactic sources from the Kim et al. (2017, 2018) sample.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The H40α (upper panel) and H36β (lower panel) integrated line intensity (moment 0, left), intensity weighted velocity (moment 1, center), and observed line-width (right) images with the 1.2 mm continuum contours overlaid for reference, with contour levels the same as in Figure 1. To make moment maps, we only used the emission above 3σ. The velocity gradient of 17 km s−1 over 3.″5 or 20 km s−1 pc−1 is detected in H40α in a roughly SE–NW direction. The size of the ALMA synthesized beam (2.″56 × 1.″95 for H40α and 0.″51 × 0.″47 for H36β) is shown in the lower left corner in each image.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The SED of 1 A showing the data points used for the fitting and with the best-fit YSO SED model from the Robitaille (2017) set overplotted. Filled circles and triangles are valid flux values and flux upper limits, respectively. The values of a reduced χ 2, interstellar visual extinction (A V), and a distance scale for the best-fit model are indicated in the plot. The icon in the upper right corner of the plot represents the basic layout of the best-fit YSO model (Robitaille 2017).
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The top panel shows the three-color image combining the HCO+ integrated intensity (red), the 1.2 mm continuum (green), and the H40α integrated intensity (blue) images with the spectral extraction regions indicated for spectra shown in the three lower panels. The H40α (unsmoothed), HCO+ (4–3), H13CO+ (3–2), and 12CO (3–2) line profiles are compared for several locations in N 105–1 A.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: From left to right, top to bottom: Band 6 H36β, H41γ, H49ϵ, H53η, and H54η recombination line integrated intensity images of N 105–1 A. The white contours in each image correspond to the 1.2 mm continuum emission with contour levels of (3, 10, 100)σ.