adsabs/AstroCLIMB huggingface dataset:
Paper: Spatially Resolved Moving Radio Burst Associated with an EUV Wave
Authors: Lei Lu, Li Feng, Weiqun Gan
Figure caption: Radio emission centroids colored by progressing time, showing the propagation direction of the radio bursts on the POS images at AIA 193 Å. The different panels correspond to the radio emission at different frequencies. The dashed line has the same meaning as that in Figure 2(f).
Paper: Spatially Resolved Moving Radio Burst Associated with an EUV Wave
Authors: Lei Lu, Li Feng, Weiqun Gan
Figure caption: Comparison of images as viewed from STEREO-B/EUVI in 195 Å (left) and SDO/AIA in 193 Å (right) at three different times (from top to bottom). The observation time of STEREO-B has been corrected by supposing that the spacecraft are located 1 au from the Sun. The inset in panel (b) shows the locations of SDO and STEREO-B in the ecliptic plane relative to the Sun. The larger dots and dashed circles in panel (d) represent the radio emission centroids and their uncertainties ( ± 0.2 R ⊙) at 150 MHz (magenta) and 228 MHz (cyan), respectively, and their projections onto the STEREO-B/EUVI images are presented in panel (c). The arrow points to an EUV wave with a coronal dimming behind.
Paper: Spatially Resolved Moving Radio Burst Associated with an EUV Wave
Authors: Lei Lu, Li Feng, Weiqun Gan
Figure caption: Kinematics of the bright coronal front. (a) Running-difference spacetime plot along the slit shown in Figure 2(f). The red dashed line represents the fifth-degree polynomial fit to the bright front. The vertical dotted line shows the start of the moving radio emission. (b) Time profile of the disk-integrated radio flux density at 150.9 MHz (black line) and the POS speed of the bright front (red line). As can be seen, the radio flux density is well correlated with the propagation speed of the bright front.
Paper: Looking at the Distant Universe with the MeerKAT Array: Discovery of a Luminous OH Megamaser at z > 0.5
Authors: Marcin Glowacki, Jordan D. Collier, Amir Kazemi-Moridani, Bradley Frank, Hayley Roberts, Jeremy Darling, Hans-Rainer Klöckner, Nathan Adams, Andrew J. Baker, Matthew Bershady, Tariq Blecher, Sarah-Louise Blyth, Rebecca Bowler, Barbara Catinella, Laurent Chemin, Steven M. Crawford, Catherine Cress, Romeel Davé, Roger Deane, Erwin de Blok, Jacinta Delhaize, Kenneth Duncan, Ed Elson, Sean February, Eric Gawiser, Peter Hatfield, Julia Healy, Patricia Henning, Kelley M. Hess, Ian Heywood, Benne W. Holwerda, Munira Hoosain, John P. Hughes, Zackary L. Hutchens, Matt Jarvis, Sheila Kannappan, Neal Katz, Dušan Kereš, Marie Korsaga, Renée C. Kraan-Korteweg, Philip Lah, Michelle Lochner, Natasha Maddox, Sphesihle Makhathini, Gerhardt R. Meurer, Martin Meyer, Danail Obreschkow, Se-Heon Oh, Tom Oosterloo, Joshua Oppor, Hengxing Pan, D. J. Pisano, Nandrianina Randriamiarinarivo, Swara Ravindranath, Anja C. Schröder, Rosalind Skelton, Oleg Smirnov, Mathew Smith, Rachel S. Somerville, Raghunathan Srianand, Lister Staveley-Smith, Masayuki Tanaka, Mattia Vaccari, Wim van Driel, Marc Verheijen, Fabian Walter, John F. Wu, Martin A. Zwaan
Figure caption: Left: RGB composite image made from the grz filters of archival Hyper Suprime-Cam (HSC) data. White contours are from the zeroth-moment map of our MeerKAT observation with no masking applied, integrated across ∼600  km s−1, at multiples of 5σ (1σ = 0.0295 Jy beam−1 km s−1). The cyan cross indicates the centroid position and uncertainties from the Franzen et al. (2015) observation with ATCA. The 14.″2 × 12.″2 MeerKAT synthesized beam is plotted as a dashed yellow ellipse. Right: spectrum of the detected OHM, with frequency Doppler-corrected to a heliocentric reference frame and rebinned from its native 26.1 kHz resolution by a factor of 2. The rest-frame velocity range included in the moment map is shaded gray; the best Gaussian fit to the OH emission profile is overlaid in blue. The red dashed line indicates the frequency (1093.7 MHz) where the 1667 MHz line would have appeared for z OH = z opt;  that z OH < z opt suggests a possible OH outflow.
Paper: Looking at the Distant Universe with the MeerKAT Array: Discovery of a Luminous OH Megamaser at z > 0.5
Authors: Marcin Glowacki, Jordan D. Collier, Amir Kazemi-Moridani, Bradley Frank, Hayley Roberts, Jeremy Darling, Hans-Rainer Klöckner, Nathan Adams, Andrew J. Baker, Matthew Bershady, Tariq Blecher, Sarah-Louise Blyth, Rebecca Bowler, Barbara Catinella, Laurent Chemin, Steven M. Crawford, Catherine Cress, Romeel Davé, Roger Deane, Erwin de Blok, Jacinta Delhaize, Kenneth Duncan, Ed Elson, Sean February, Eric Gawiser, Peter Hatfield, Julia Healy, Patricia Henning, Kelley M. Hess, Ian Heywood, Benne W. Holwerda, Munira Hoosain, John P. Hughes, Zackary L. Hutchens, Matt Jarvis, Sheila Kannappan, Neal Katz, Dušan Kereš, Marie Korsaga, Renée C. Kraan-Korteweg, Philip Lah, Michelle Lochner, Natasha Maddox, Sphesihle Makhathini, Gerhardt R. Meurer, Martin Meyer, Danail Obreschkow, Se-Heon Oh, Tom Oosterloo, Joshua Oppor, Hengxing Pan, D. J. Pisano, Nandrianina Randriamiarinarivo, Swara Ravindranath, Anja C. Schröder, Rosalind Skelton, Oleg Smirnov, Mathew Smith, Rachel S. Somerville, Raghunathan Srianand, Lister Staveley-Smith, Masayuki Tanaka, Mattia Vaccari, Wim van Driel, Marc Verheijen, Fabian Walter, John F. Wu, Martin A. Zwaan
Figure caption: Predicted distributions of gas-rich mergers traced by OH at z OH ∼ 0.52 (blue), and H I-rich disk galaxies at z H I ∼ 0.30 (red), in WISE color–magnitude and color–color space, generated using algorithms presented in Roberts et al. (2021). Contours enclose the upper 99% (dashed), 90%, 80%,…, 20%, and 10% of the Gaussian kernel density estimates for the respective galaxy distributions. In the left panel, both OH and H I identifications are supported for LADUMA J033046.20−275518.1, while in the right panel, OH is clearly preferred.
Paper: Looking at the Distant Universe with the MeerKAT Array: Discovery of a Luminous OH Megamaser at z > 0.5
Authors: Marcin Glowacki, Jordan D. Collier, Amir Kazemi-Moridani, Bradley Frank, Hayley Roberts, Jeremy Darling, Hans-Rainer Klöckner, Nathan Adams, Andrew J. Baker, Matthew Bershady, Tariq Blecher, Sarah-Louise Blyth, Rebecca Bowler, Barbara Catinella, Laurent Chemin, Steven M. Crawford, Catherine Cress, Romeel Davé, Roger Deane, Erwin de Blok, Jacinta Delhaize, Kenneth Duncan, Ed Elson, Sean February, Eric Gawiser, Peter Hatfield, Julia Healy, Patricia Henning, Kelley M. Hess, Ian Heywood, Benne W. Holwerda, Munira Hoosain, John P. Hughes, Zackary L. Hutchens, Matt Jarvis, Sheila Kannappan, Neal Katz, Dušan Kereš, Marie Korsaga, Renée C. Kraan-Korteweg, Philip Lah, Michelle Lochner, Natasha Maddox, Sphesihle Makhathini, Gerhardt R. Meurer, Martin Meyer, Danail Obreschkow, Se-Heon Oh, Tom Oosterloo, Joshua Oppor, Hengxing Pan, D. J. Pisano, Nandrianina Randriamiarinarivo, Swara Ravindranath, Anja C. Schröder, Rosalind Skelton, Oleg Smirnov, Mathew Smith, Rachel S. Somerville, Raghunathan Srianand, Lister Staveley-Smith, Masayuki Tanaka, Mattia Vaccari, Wim van Driel, Marc Verheijen, Fabian Walter, John F. Wu, Martin A. Zwaan
Figure caption:  L OH vs. L FIR for known OHMs (H. Roberts et al. 2022, in preparation). LADUMA J033046.20−275518.1 (green star) is one of the most luminous OHMs on both axes.
Paper: Looking at the Distant Universe with the MeerKAT Array: Discovery of a Luminous OH Megamaser at z > 0.5
Authors: Marcin Glowacki, Jordan D. Collier, Amir Kazemi-Moridani, Bradley Frank, Hayley Roberts, Jeremy Darling, Hans-Rainer Klöckner, Nathan Adams, Andrew J. Baker, Matthew Bershady, Tariq Blecher, Sarah-Louise Blyth, Rebecca Bowler, Barbara Catinella, Laurent Chemin, Steven M. Crawford, Catherine Cress, Romeel Davé, Roger Deane, Erwin de Blok, Jacinta Delhaize, Kenneth Duncan, Ed Elson, Sean February, Eric Gawiser, Peter Hatfield, Julia Healy, Patricia Henning, Kelley M. Hess, Ian Heywood, Benne W. Holwerda, Munira Hoosain, John P. Hughes, Zackary L. Hutchens, Matt Jarvis, Sheila Kannappan, Neal Katz, Dušan Kereš, Marie Korsaga, Renée C. Kraan-Korteweg, Philip Lah, Michelle Lochner, Natasha Maddox, Sphesihle Makhathini, Gerhardt R. Meurer, Martin Meyer, Danail Obreschkow, Se-Heon Oh, Tom Oosterloo, Joshua Oppor, Hengxing Pan, D. J. Pisano, Nandrianina Randriamiarinarivo, Swara Ravindranath, Anja C. Schröder, Rosalind Skelton, Oleg Smirnov, Mathew Smith, Rachel S. Somerville, Raghunathan Srianand, Lister Staveley-Smith, Masayuki Tanaka, Mattia Vaccari, Wim van Driel, Marc Verheijen, Fabian Walter, John F. Wu, Martin A. Zwaan
Figure caption: Independent velocity channel maps of an 8× rebinned 26.1 kHz data cube, with velocities indicated relative to our measured systemic redshift of z OH = 0.5225. Contours are multiples of 2σ (1σ = 0.283 mJy beam−1). The 14.″2 × 12.″2 synthesized beam is plotted in the top-left panel.
Paper: Solar-like Dynamos and Rotational Scaling of Cycles from Star-in-a-box Simulations
Authors: Petri J. Käpylä
Figure caption: Ratios of rotation to cycle period as a function of Co with ﹩{P}_{\mathrm{rot}}/{P}_{\mathrm{cyc}}^{\mathrm{surf}}﹩ (black) and ﹩{P}_{\mathrm{rot}}/{P}_{\mathrm{cyc}}^{\mathrm{deep}}﹩ (gray). Additional data are from Warnecke (2018; red), Strugarek et al. (2018; blue), and Guerrero et al. (2019; brown). The dotted lines show power-law fits to the data (a). The solar data point (⊙) is computed using data from Brandenburg et al. (2017) with Co = 2π τ/P rot, where τ is the convective turnover time. Panel (b) shows the ratio E mag/E kin as a function of Co from the same studies. Fits to full data (dotted lines) and subsets (dashed lines) where some data are omitted are shown (see text).
Paper: The Age of Discovery with the James Webb Space Telescope: Excavating the Spectral Signatures of the First Massive Black Holes
Authors: Kohei Inayoshi, Masafusa Onoue, Yuma Sugahara, Akio K. Inoue, Luis C. Ho
Figure caption: Redshift evolution of the broadband colors used for selecting high-z seed BHs (black) at z ∼ 8 (left) and z ∼ 10 (right). For comparison, we also plot those for other three types of high-z sources: quasars (cyan), Population III galaxies (blue), and star-forming galaxies with Z = Z ⊙ (green) with stellar age of 10 (solid), 100 (dashed), and 500 (dotted) Myr. The quasar SED model assumes a power-law continuum with a UV slope of ﹩{\alpha }_{\lambda }\equiv d\mathrm{ln}{f}_{\lambda }/d\mathrm{ln}\lambda =-1.70﹩ (Selsing et al. 2016) and various broad emission lines, the strength of which is based on a low-z measurement by Vanden Berk et al. (2001). The galaxy SEDs are from Inoue (2011). In those four panels, the broadband colors of seed BHs are generally red compared to those of galaxies that have bluer UV continua. The colors sharply increase (or decrease) when the prominent Hα emission enters the longer-wavelength (shorter-wavelength) filters. The combination of the red continuum and extremely strong Hα makes the F356W − F560W and F444W − F770W colors of the growing seed BHs as large as ≳1. Note that the sharp rise of the F200W – F356W color at z > 14 is due to IGM absorption.
Paper: The Age of Discovery with the James Webb Space Telescope: Excavating the Spectral Signatures of the First Massive Black Holes
Authors: Kohei Inayoshi, Masafusa Onoue, Yuma Sugahara, Akio K. Inoue, Luis C. Ho
Figure caption: SED of the growing seed BH with M • ≃ 106 M ⊙ at z = 8: the total SED (blue), the radiation flux from the nuclear BH with nebular emission lines (magenta), and the emission from the dense accretion disk at r ∼ 0.1–1 pc (green). The viewing angle is set to θ obs = 60°. The imaging sensitivity curves with S/N = 10 of JWST’s NIRCam (0.6–5 μm) and MIRI (5–20 μm) in a 10 ks exposure time are overlaid (the open square symbol indicates the effective wavelength of each filter), along with the transmission curve of each filter at the bottom (arbitrary units). The filled square symbols present the filter-convolved flux density at each filter. The continuum radiation flux with several prominent lines with the rest-frame equivalent widths of EWrest > 7 Å is observable with the NIRCam broadband filters except for F070W and the MIRI F560W filter. Intergalactic medium (IGM) absorption is not explicitly included but becomes important in the shaded region at λ obs < 1.09 μm.
Paper: The Age of Discovery with the James Webb Space Telescope: Excavating the Spectral Signatures of the First Massive Black Holes
Authors: Kohei Inayoshi, Masafusa Onoue, Yuma Sugahara, Akio K. Inoue, Luis C. Ho
Figure caption: Density structure of the accretion flow onto a seed BH and a schematic picture describing our SED modeling, which includes three components: (1) the radiation flux produced from the unresolved nuclear disk of the BH, (2) nebular emission lines emitted from irradiated gas parcels, and (3) radiation from the dense accreting disk in the RHD simulation domain. The physical quantities of n, T, U, x e, Δs, and θ obs are the number density of hydrogen nuclei, gas temperature, ionization parameter, electron fraction, thickness of gas parcels, and viewing angle, respectively. The quantities with brackets 〈 · 〉 are the mass-weighted values along the vertical direction (see more details in the text). The boundary between the nebula and disk is defined by x e = 0.9 (thin curve).
Paper: The Warm Neptune GJ 3470b Has a Polar Orbit
Authors: Guđmundur Stefànsson, Suvrath Mahadevan, Cristobal Petrovich, Joshua N. Winn, Shubham Kanodia, Sarah C. Millholland, Marissa Maney, Caleb I. Cañas, John Wisniewski, Paul Robertson, Joe P. Ninan, Eric B. Ford, Chad F. Bender, Cullen H. Blake, Heather Cegla, William D. Cochran, Scott A. Diddams, Jiayin Dong, Michael Endl, Connor Fredrick, Samuel Halverson, Fred Hearty, Leslie Hebb, Teruyuki Hirano, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Michael W. McElwain, Andrew J. Metcalf, Andrew Monson, Jayadev Rajagopal, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Heidi Schweiker, Ryan C. Terrien, Jason T. Wright
Figure caption: Top panels: diffuser-assisted transit observations with the ARCTIC imager on the ARC 3.5 m Telescope at Apache Point Observatory on (a) 2019 December 2 and (b) 2019 December 22. The best-fit model is shown in red, unbinned data are shown in black, and 5 minute binned data are shown with the blue points. Lower panels: RM effect of GJ 3470b as observed by NEID on (c) 2021 January 2 UT and (d) 2021 January 12 UT. The best-fit joint model of both RM observations (red) results in a sky-projected obliquity of ﹩\lambda ={98}_{-12}^{+15\circ }﹩. The red regions show the 1σ credible intervals. The expected well-aligned model is shown with the gray dashed lines, which assumes ψ = 0°, i.e., that ﹩v\sin i={v}_{\mathrm{eq}}﹩, and λ = 0°. Both observations disfavor the well-aligned model. The RVs and diffuser-assisted photometry are available as data behind the figure.(The data used to create this figure are available.)
Paper: The Warm Neptune GJ 3470b Has a Polar Orbit
Authors: Guđmundur Stefànsson, Suvrath Mahadevan, Cristobal Petrovich, Joshua N. Winn, Shubham Kanodia, Sarah C. Millholland, Marissa Maney, Caleb I. Cañas, John Wisniewski, Paul Robertson, Joe P. Ninan, Eric B. Ford, Chad F. Bender, Cullen H. Blake, Heather Cegla, William D. Cochran, Scott A. Diddams, Jiayin Dong, Michael Endl, Connor Fredrick, Samuel Halverson, Fred Hearty, Leslie Hebb, Teruyuki Hirano, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Michael W. McElwain, Andrew J. Metcalf, Andrew Monson, Jayadev Rajagopal, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Heidi Schweiker, Ryan C. Terrien, Jason T. Wright
Figure caption: (a) S HK as a function of the residual RV from Model II. The residual RV includes the RV slope (see Figure 2(b)). (b) Hα index as a function of residual RV. The Spearman’s rank correlation coefficient ρ for each data set is shown in the legends. We see no clear correlations between S HK or Hα with the residual RVs. (c) Lomb–Scargle periodograms of (i) the S HK indicator from HARPS, (ii) S HK indicator from HIRES, (iii) Hα indicator from HARPS, and (iv) residual RV (slope removed) from HARPS, HIRES, and HPF. The known stellar rotation period is shown with the red dashed line. The orange horizontal lines show the 10% (solid line) and the 1% (dotted–dashed line) false-alarm probabilities calculated with the bootstrap method.
Paper: The Warm Neptune GJ 3470b Has a Polar Orbit
Authors: Guđmundur Stefànsson, Suvrath Mahadevan, Cristobal Petrovich, Joshua N. Winn, Shubham Kanodia, Sarah C. Millholland, Marissa Maney, Caleb I. Cañas, John Wisniewski, Paul Robertson, Joe P. Ninan, Eric B. Ford, Chad F. Bender, Cullen H. Blake, Heather Cegla, William D. Cochran, Scott A. Diddams, Jiayin Dong, Michael Endl, Connor Fredrick, Samuel Halverson, Fred Hearty, Leslie Hebb, Teruyuki Hirano, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Michael W. McElwain, Andrew J. Metcalf, Andrew Monson, Jayadev Rajagopal, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Heidi Schweiker, Ryan C. Terrien, Jason T. Wright
Figure caption: Polar Neptunes: sky-projected obliquities (λ; upper panel) and true obliquities (ψ; lower panel; when available) as a function of stellar effective temperature. Planets either similar in radius or mass to Neptune (1.5R ⊕ < R < 6R ⊕ or 10M ⊕ < M < 50M ⊕) on circular orbits are highlighted in blue, and Neptunes on eccentric orbits (e > 0.1 and >2σ discrepant from e = 0) are shown in red. Other systems from Albrecht et al. (2021) are shown in gray. We show WASP-107b as both red and blue, as it formally has an eccentricity constraint of e = 0.06 ± 0.04 and Piaulet et al. (2021) mention it could have a moderate eccentricity. GJ 3470b joins a growing sample of warm Neptunes orbiting cool stars on polar orbits. Data obtained from Albrecht et al. (2021), TEPCAT (Southworth 2011), and the NASA Exoplanet archive (Akeson et al. 2013).
Paper: The Warm Neptune GJ 3470b Has a Polar Orbit
Authors: Guđmundur Stefànsson, Suvrath Mahadevan, Cristobal Petrovich, Joshua N. Winn, Shubham Kanodia, Sarah C. Millholland, Marissa Maney, Caleb I. Cañas, John Wisniewski, Paul Robertson, Joe P. Ninan, Eric B. Ford, Chad F. Bender, Cullen H. Blake, Heather Cegla, William D. Cochran, Scott A. Diddams, Jiayin Dong, Michael Endl, Connor Fredrick, Samuel Halverson, Fred Hearty, Leslie Hebb, Teruyuki Hirano, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Michael W. McElwain, Andrew J. Metcalf, Andrew Monson, Jayadev Rajagopal, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Heidi Schweiker, Ryan C. Terrien, Jason T. Wright
Figure caption: Corner plot of the posteriors of λ, v eq, i ⋆, ﹩v\sin i﹩, and ψ. The posteriors for the true obliquity are ﹩\psi ={95}_{-8}^{+9\circ }﹩, and are compatible with 90° for any posterior value of ﹩v\sin i﹩.
Paper: The Warm Neptune GJ 3470b Has a Polar Orbit
Authors: Guđmundur Stefànsson, Suvrath Mahadevan, Cristobal Petrovich, Joshua N. Winn, Shubham Kanodia, Sarah C. Millholland, Marissa Maney, Caleb I. Cañas, John Wisniewski, Paul Robertson, Joe P. Ninan, Eric B. Ford, Chad F. Bender, Cullen H. Blake, Heather Cegla, William D. Cochran, Scott A. Diddams, Jiayin Dong, Michael Endl, Connor Fredrick, Samuel Halverson, Fred Hearty, Leslie Hebb, Teruyuki Hirano, Andrea S. J. Lin, Sarah E. Logsdon, Emily Lubar, Michael W. McElwain, Andrew J. Metcalf, Andrew Monson, Jayadev Rajagopal, Lawrence W. Ramsey, Arpita Roy, Christian Schwab, Heidi Schweiker, Ryan C. Terrien, Jason T. Wright
Figure caption: Fit of out-of-transit RVs of GJ 3470 with the known orbit of GJ 3470b, a linear slope, and a quasi-periodic GP model. HARPS RVs before and after the 2015 fiber break are shown in yellow (denoted HARPS1) and purple (denoted HARPS2), respectively, HIRES RVs are shown in black, and HPF RVs in pink. (a) RVs as a function of time. (b) Residuals including the RV slope. (c) Phase-folded RVs. The RVs are available as machine-readable data behind the figure.(The data used to create this figure are available.)
Paper: Discovery of a 500 au Protobinary in the Massive Prestellar Core G11.92–0.61 MM2
Authors: C. J. Cyganowski, J. D. Ilee, C. L. Brogan, T. R. Hunter, S. Zhang, 遂楠 张, T. J. Harries, T. J. Haworth
Figure caption: (a)–(c): ALMA 1.3 mm continuum images made with robust parameters of (a) R = 1.0, (b) R = 0.0, and (c) R = −1.0, with millimeter sources labeled in (c). (d)–(f): R = −1.0 images of (d) the two compact components only, (e) the diffuse component only, and (f) the residual of the simultaneous three-component fit (Section 3.1). (d) and (f) also show contours of the image shown in color scale, levels: (d) [10] × σ (yellow), (f) [4,7] × σ (solid white), [−4] × σ (dashed white), σ = 7.4e−5 Jy beam−1. (g)–(h): ALMA 1.3 mm (g) and VLA 0.9 cm (h) images convolved to a common beam (0.″280 × 0.″155, PA = −6.°2). (i): spectral index image created from (g) and (h), masked at the 5σ level. Panels (d)–(f) are displayed using a common color scale, shown to the right of (f); panels (a)–(c) and (g)–(h) similarly use a power-law stretch with exponent = 0.9 and a minimum of 0.0, but with the maximum set to the peak value for MM2 of each individual image. Contours of the R = −1.0 Planck T  b  image are overplotted in cyan in (c) and (e)–(f) and in black in (i), levels: [25, 40, 55 K]. The synthesized beam is shown at the lower left in each panel.
Paper: Discovery of a 500 au Protobinary in the Massive Prestellar Core G11.92–0.61 MM2
Authors: C. J. Cyganowski, J. D. Ilee, C. L. Brogan, T. R. Hunter, S. Zhang, 遂楠 张, T. J. Harries, T. J. Haworth
Figure caption: (a): Zoom of MM2 showing the minimum map of the 13CO J = 2–1 absorption. The white 10σ continuum contour from Figure 1(d) shows the “bridge” (Section 3.1). Crosses mark pixels for which spectra are shown. (b)–(d): 13CO J = 2–1 spectra (black) at the fitted continuum positions of MM2E and MM2W and a “bridge” pixel, overplotted with Gaussian fits to the line core (red; the MM2W fit excludes the channels shown with a dotted line). The estimated systemic velocity (37 km s−1, Section 3.4) is shown as a dashed gray line; labels give best-fit parameters. (e): 1.3 mm Planck T  b  (R = −1) image overlaid with contours of integrated red/blueshifted CH3OH 4−1,3–30,3 emission. Levels: [4,7] × σ = 3.3 mJy beam−1 km s−1 (red), [4, 7, 10, 15] × σ = 5.5 mJy beam−1 km s−1 (blue). (f): Proposed morphology of MM2, viewed perpendicular to the line of sight. (a) and (e): ALMA synthesized beams are shown at the bottom left.
Paper: Discovery of a 500 au Protobinary in the Massive Prestellar Core G11.92–0.61 MM2
Authors: C. J. Cyganowski, J. D. Ilee, C. L. Brogan, T. R. Hunter, S. Zhang, 遂楠 张, T. J. Harries, T. J. Haworth
Figure caption: Channel maps showing CH3OH 4−1,3–30,3 (color scale and gray contour, 4 × σ = 1.2 mJy beam−1) and H2CO 40,4–30,3 (white contours, [4,7,10,15] × σ = 4.9 mJy beam−1) emission. Red circles mark the positions of MM2E and MM2W (Table 2).
Paper: GRB 200826A: A Precursor of a Long Gamma-Ray Burst with Missing Main Emission
Authors: Xiangyu Ivy Wang, Bin-Bin Zhang, Wei-Hua Lei
Figure caption: Top: light curve of GRB 160625B. Middle: The solid red line is the light curve of GRB 200826A. The dashed red line is the assumed ME of the prototype burst. Bottom: The solid blue line shows how the viewing angle ψ(t) changes over time, and the dashed black line is the jet-opening angle. The gray shaded area is where the ME can be missed by the observer.
Paper: GRB 200826A: A Precursor of a Long Gamma-Ray Burst with Missing Main Emission
Authors: Xiangyu Ivy Wang, Bin-Bin Zhang, Wei-Hua Lei
Figure caption: Comparison of the spectral evolution between GRB 200826A and the precursor of GRB 160625B. Both bursts are fitted by the cutoff power law (CPL) model. The bottom panel shows the comparison of the light curves of the two events. Data are taken from Zhang et al. (2018) and Zhang et al. (2021).
Paper: GRB 200826A: A Precursor of a Long Gamma-Ray Burst with Missing Main Emission
Authors: Xiangyu Ivy Wang, Bin-Bin Zhang, Wei-Hua Lei
Figure caption: The schematic sketch of the companion-obstruction model. See also Zou et al. (2021). (a) The configuration of the system during the precursor phase. (b) The configuration for the ME phase.