adsabs/AstroCLIMB huggingface dataset:
Paper: Star and Cluster Formation in the Sh2-112 Filamentary Cloud Complex
Authors: Alik Panja, Yan Sun, Wen Ping Chen, Soumen Mondal
Figure caption: The H2 column density distribution for 12CO (a), 13CO (b), and C18O (c), respectively.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Graphs of (a) and (c) magnetic energy and (b) and (d) volume-integrated electric current. Graphs (a) and (b) show the magnetic energy and volume-integrated electric current as a function of time for the simulations using the bipoles determined from the high-cadence (AFT maps, solid lines) and low-cadence (HMI Carrington maps, dashed lines). The legend in graph (b) describes the line styles and colors, where in each case black denotes the ideal simulations (IdealA0 and IdealH0), green the simulations with ohmic dissipation (OhmA0 and OhmH0), blue the simulations with Hyper Diffusion (HDA0 and HDH0), and red simulations with Statistically Averaged Helicity Condensation (SAHCA1 and SAHCH1). For all of the simulations, the bipoles are inserted with zero twist. Graphs (c) and (d) show the magnetic energy and volume electric current on 2015 March 20 for all simulations. The diamonds denote the simulations using bipoles determined from the AFT data, and the stars the simulations using bipoles determined from HMI Carrington rotation synoptic maps. Black has the bipole twist parameter β = 0, blue β = 0.2, green β = 0.4, and red β = 0.6. The light blue and yellow colors denote supergranular vorticity of 1 × 10−6 s−1 (light blue) and 5 × 10−6 s−1 (yellow).
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Comparison of the field lines at the locations of the observed filaments. (a) Hα from BBSO taken on 2015 March 20 at 1845UT, where eight filaments are labeled. Panels (b)–(i) present the results for runs. (b) OhmA4: eight filaments, (c) OhmH4: seven filaments, (d) HDA4: three filaments, (e) IdealA4: six filaments, (f) OhmA0: five filaments, (g) HDA0: three filaments, (h) IdealA0: five filaments, and (i) SHGIA1, five filaments. In each of panels (b)–(i), white and back respectively represent positive and negative flux, where the values saturate at ±20 G. All of the simulation results are derived from using the AFT high-cadence bipole data, except for panel (c), which uses the lower-cadence HMI bipole data.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: (a) PROBA2/SWAP 174 Å image taken on the 2015 March 20 at 12:00UT, showing the large-scale off-limb structure of the solar corona. The off-limb structures have been divided into six regions where regions A and E denote faint open fields, while regions B, C, D, and F contain a mixture of bright closed corona loops in addition to faint open fields. Panels (b)–(f) show the results for the plane-of-sky magnetic fields for (b) HDA2, (c) OhmA2, (d) IdealA2, (e) HDH2, and (f) SAHCA1. For each of panels (b)–(f), positive/negative flux is given by white/black, where the field values saturate at ±20 G and the colored lines are the field lines.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Distributions of the radial magnetic field (B  r ) at 2.5 solar radii for a PFSS extrapolations (a and b) and non-potential simulations (c–f). The left/right-hand columns show results from the high/low-cadence bipole data sets. The middle row shows results from simulations (c) OhmA4 and (d) OhmH4, while the bottom row shows results from (e) SAHCA5 and (f) SAHCH5. In each plot, red/blue represents positive/negative B  r . The fields saturate at ±0.4 G.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Scatter plots of the amount of open flux on 2015 March 20 for all of the simulations. The diamonds denote the simulations using bipoles determined from the high-cadence data set, while the stars denote the simulations using the low-cadence data set. Black color denotes a bipole twist parameter β = 0, blue β = 0.2, green β = 0.4, and red β = 0.6. The light blue and yellow colors denote a vorticity rate of 1 × 10−6 (light blue) and 5 × 10−6 (yellow). The solid horizontal line gives the OMNI 27-day average. The full length black/purple horizontal dash/dashed–dotted lines show the open flux deduced from a PFSS model with source surface at 2.5R ⊙ for the high-/low-cadence data sets. Results for reducing the source surface of the PFSS model to either 2.2R ⊙ (plus) or 2.0R ⊙ (triangles) are also included for the high-cadence (black) and low-cadence (purple) data sets. The partial length black (high-cadence)/purple(low-cadence) horizontal dashed/dashed–dotted lines give the open flux deduced from a PFSS model (2.5R ⊙) when the radial outflow velocity is included.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Scatter plot of the number of filament locations reproduced by the simulations, based on the coronal physics included. The diamonds denote the simulations using bipoles determined from the AFT simulations, and the stars the simulations using bipoles determined from HMI Carrington rotation synoptic maps. Black color denotes a bipole twist parameter β = 0, blue β = 0.2, green β = 0.4, and red β = 0.6. The light blue and yellow colors denote supergranular helicity injection at respective rates of 1 × 10−6 s−1 (light blue) and 5 × 10−6 s−1 (yellow). The horizontal dashed line denotes the number of observed filaments.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Graphs of the variation of the open flux as a function of time for (a) ideal (IdealA0 and IdealH0; shown in black) and supergranular helicity injection (SAHCA1 and SAHCH1, red) simulations and (b) simulations with ohmic dissipation (OhmA0 and OhmH0, green) and with hyperdiffusion (HDA0 and HDH0; shown in blue). In each graph, results are shown for the simulations using the high-cadence bipoles (solid lines) and low-cadence bipoles (dashed lines). For all of the simulations, the bipoles are inserted with zero twist. The vertical dashed line denotes the date of the eclipse.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Distribution of open and closed field lines at the solar photosphere for PFSS extrapolations (a and b) and non-potential simulations (c–f). The left-/right-hand columns show results from the high-/low-cadence bipole data sets. The middle row shows results from simulations (c) OhmA4 and (d) OhmH4, while the bottom row shows results from (e) SAHCA5 and (f) SAHCH5. In each plot, red/blue represent positive/negative B  r  open footpoints. The green locations represent closed field at the solar surface.
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: Variation of the photospheric flux over the 210 days of the simulation from 2014 September 1 to 2015 March 30. The solid line denotes the simulation using bipoles determined from the AFT magnetograms, while the dashed line is for bipoles determined from HMI Carrington rotation synoptic maps. The triangles denote the surface flux computed from both the AFT magnetograms (blue) and HMI Carrington rotation maps (red). The horizontal red and blue lines denote the time period over which the flux is calculated in each data set. The vertical dotted line gives the time of the eclipse on 2015 March 20.
Paper: An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt Law
Authors: Louise Breuval, Adam G. Riess, Pierre Kervella, Richard I. Anderson, Martino Romaniello
Figure caption: The PL intercept (β) in the W  JK  Wesenheit index fitted with a common slope in the MW, LMC, and SMC as a function of the mean metallicity ([Fe/H]) of the galaxy (Equation (4)).
Paper: An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt Law
Authors: Louise Breuval, Adam G. Riess, Pierre Kervella, Richard I. Anderson, Martino Romaniello
Figure caption: Top: PL slope (α) in the MW and Magellanic Clouds represented with the inverse of wavelength. Bottom: PL intercept (β) obtained in the MW and Magellanic Clouds with a slope fixed to that of the LMC, represented with the inverse of wavelength.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: (a) The time series of the Sun-as-a-star Hα spectra (dynamic spectrum) and (b) the light curves of event (1), the C8.0 flare on 2017 April 2. In panel (a), the left vertical axis is the difference in wavelength from the Hα line center in units of Angstrom, and the right vertical axis is the corresponding Doppler velocity in units of kilometers per second. The horizontal axis is the time measured from 02:30 UT on 2017 April 2 in units of minutes. The color map shows ΔS(t, λ), where ΔS(t, λ) represents the ratio of the changes in the pre-event-subtracted spatially integrated Hα spectra to the full-disk continuum (see Equation (5)). The orange and purple regions correspond to emission and absorption, respectively. In the gray regions, there is no available data. Panel (b) shows the differenced equivalent widths of Hα ± 3.0  Å as red circles and the GOES soft X-ray (1−8 Å) flux plotted as a blue dashed line. The horizontal axis is the same as that in panel (a). The horizontal dashed line represents the zero level of differenced equivalent width.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: Overview of event (4), which occurred on 2021 April 19–20. (a) A full-disk solar image at the Hα-center wavelength observed by SMART/SDDI. Celestial north is up, and west is to the right. The orange dashed−dotted region corresponds to the images in Figure 7(b), and the inner red dashed region is a TR. The blue solid region is a QR. The direction of the solar north is shown by the white arrow labeled SN. (b) The time evolution of the M1.1 class flare on 2021 April 19. The field of view in each panel corresponds to the orange dashed−dotted region in Figure 7(a). In each row, images at the times t = 17, 35, and 66 minutes measured from 23:30 UT on 2021 April 19 are shown from top to bottom. In each column, the images AIA 171 Å, AIA 131 Å, Hα − 1.0 Å, Hα center, and Hα + 1.0 Å are shown from left to right. The red dashed region indicated in the Hα center image at t = 17 minutes is a TR. The pink arrow indicates plasma downflow during the decay phase of this M1.1 flare.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: Overview of event (3), which occurred on 2017 September 8. (a) A full-disk solar image at the Hα-center wavelength observed by SMART/SDDI. Celestial north is up, and west is to the right. The red dashed is a TR, and the blue solid region is a QR. The direction of the solar north is shown by the white arrow labeled SN. (b) The time evolution of the M8.1 flare on 2017 September 8. The field of view in each panel corresponds to the TR in Figure 5(a). In each row, images at the times t = 18, 56, and 62 minutes measured from 07:30 UT on 2017 September 8 are shown from top to bottom. In each column, the images AIA 171 Å, AIA 131 Å, Hα − 1.0 Å, Hα center, and Hα + 1.0 Å are shown from left to right. The pink arrows indicate plasma eruptions associated with the second brightening.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: Overview of event (2), which occurred on 2017 April 2. (a) A full-disk solar image at the Hα-center wavelength observed by SMART/SDDI. The red dashed region is a TR, and the blue solid region is a QR. Celestial north is up, and west is to the right. The direction of the solar north is shown by the white arrow labeled SN. (b) The time evolution of the M5.3 flare on 2017 April 2. The field of view in each panel corresponds to the TR in Figure 3(a). In each row, images at the times t = 25, 33, and 60 minutes measured from 07:30 UT on 2017 April 2 are shown from top to bottom. In each column, the images AIA 171 Å, AIA 131 Å, Hα − 1.0 Å, Hα center, and Hα + 1.0 Å are shown from left to right.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: Overview of event (1), which occurred on 2017 April 2. (a) A full-disk solar image at the Hα-center wavelength observed by SMART/SDDI. Celestial north is up, and west is to the right. The red dashed region is a TR, and the blue solid region is a QR. The direction of the solar north is shown by the white arrow labeled SN. (b) The time evolution of the C8.0 flare on 2017 April 2. The field of view in each panel corresponds to the TR in Figure 1(a). In each row, the images at the times t = 15, 17, 30, and 40 minutes measured from 02:30 UT on 2017 April 2 are shown from top to bottom. In each column, the images AIA 171 Å, AIA 131 Å, Hα − 1.0 Å, Hα center, and Hα + 1.0 Å are shown from left to right.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: The same as Figure 2, but for event (2), the M5.3 flare on 2017 April 2. We note that only Hα ± 3.0 Å data were available for performing the Sun-as-a-star analysis in this event.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: The same as Figure 2, but for event (4), the M1.1 flare on 2021 April 19−20.
Paper: Sun-as-a-star Analyses of Various Solar Active Events Using Hα Spectral Images Taken by SMART/SDDI
Authors: Takato Otsu, Ayumi Asai, Kiyoshi Ichimoto, Takako T. Ishii, Kosuke Namekata
Figure caption: The same as Figure 2, but for event (3), the M8.1 flare on 2017 September 8. We note that only Hα ± 3.0 Å data were available for performing the Sun-as-a-star analysis in this event.
Paper: Star and Cluster Formation in the Sh2-112 Filamentary Cloud Complex
Authors: Alik Panja, Yan Sun, Wen Ping Chen, Soumen Mondal
Figure caption: Color–color diagrams of Class I (red squares), Class II (green triangles), transition-disk (blue circles), and nonexcess (gray dots) sources, identified by complementary classification schemes (Koenig et al. 2012). In each scheme, the dotted lines denote the adopted color criteria. (a) Class I and Class II objects are selected by the WISE 3.4, 4.6, and 12 μm colors. (b) Heavily embedded sources are recognized by a combination of WISE 3.4 and 4.6 μm, and UKIDSS data. Sources are dereddened in this analysis. Sources that are already found in the previous scheme are shown as open symbols, whereas the additional candidates selected in this scheme are solid symbols, and a similar sequence is followed for the consecutive plots. (c) This WISE color–color diagram plots all the YSOs identified consistently with three analysis schemes, including the transition-disk objects recognized by WISE 3.4, 4.6, and 22 μm data. (d) Distribution of all the YSOs identified in the previous schemes along with the additional Class I and Class II sources identified only using the excess emission in the UKIDSS bands. The solid blue and red lines mark the locus of dwarfs and giants, both taken from Bessell & Brett (1988), and the solid black line indicates the CTTs locus, taken from Meyer et al. (1997). The three parallel dashed lines represent the reddening vectors. All the photometric data points in this figure are converted to the CIT (Elias et al. 1982) system.
Paper: Star and Cluster Formation in the Sh2-112 Filamentary Cloud Complex
Authors: Alik Panja, Yan Sun, Wen Ping Chen, Soumen Mondal
Figure caption: The IPHAS r − Hα vs. r − i color–color diagram to select Hα emission stars. Candidate Hα emitters are represented by magenta diamonds, whereas the field interlopers are depicted as gray dots. The solid and dashed blue lines represent the unreddened main sequence, which normally serves as the upper bound to the main stellar locus, and the expected position of unreddened main-sequence stars with Hα emission strengths of an equivalent width of −10 Å. The nearly vertical solid black and green lines show the trend for an unreddened Rayleigh–Jeans continuum and the unreddened continuum of an F0 spectral type, respectively. The black broken lines are the predicted lines of constant net emission.
Paper: Star and Cluster Formation in the Sh2-112 Filamentary Cloud Complex
Authors: Alik Panja, Yan Sun, Wen Ping Chen, Soumen Mondal
Figure caption: The extinction map around S112 computed by the H- and K-band photometry with a grid size of 30″ × 30″. The dashed circle marks the 15′ radius around S112. Enhanced extinction is seen generally in a zone in the Galactic east–west direction, with a multitude of dense clumps where extinction exceeds A  K  ∼ 1.55 mag, or A  V  ≳ 17 mag. A 10 pc linear scale is displayed, assuming a heliocentric distance of 2.1 kpc to the complex.
Paper: Pulse Timing Discovery of a Three-day Companion to the Hot Subdwarf BPM 36430
Authors: Bryce A. Smith, Brad N. Barlow, Benjamin Rosenthal, J. J. Hermes, Veronika Schaffenroth
Figure caption: Lomb–Scargle periodogram of the 20 s cadence TESS light curve of BPM 36430, zoomed in on the dominant pulsation mode (top). Also shown are the periodograms after subtracting a fixed sinusoid (middle) and a phase-modulated sinusoid from the data (bottom). The dashed vertical lines mark position of the pulsation mode (black) and the two equidistant splittings (orange) arising from the orbital frequency of 0.32 cycles per day.
Paper: Pulse Timing Discovery of a Three-day Companion to the Hot Subdwarf BPM 36430
Authors: Bryce A. Smith, Brad N. Barlow, Benjamin Rosenthal, J. J. Hermes, Veronika Schaffenroth
Figure caption: Spectral energy distribution of BPM 36430 and our model fit, which shows that a ≈29,000 K sdB star dominates the light from the system.
Paper: Pulse Timing Discovery of a Three-day Companion to the Hot Subdwarf BPM 36430
Authors: Bryce A. Smith, Brad N. Barlow, Benjamin Rosenthal, J. J. Hermes, Veronika Schaffenroth
Figure caption: Lomb–Scargle periodogram of the full, 2 minutes cadence TESS light curve of BPM 36430 showing a strong radial-mode pulsation and an inset of g-mode pulsations (top). A dashed red line denotes the 5.1σ level, which corresponds to a false alarm probability of 0.1%. Also shown is the 20 s cadence light curve phase-folded on the dominant pulsation mode at 341.6734767 s (bottom).
Paper: Pulse Timing Discovery of a Three-day Companion to the Hot Subdwarf BPM 36430
Authors: Bryce A. Smith, Brad N. Barlow, Benjamin Rosenthal, J. J. Hermes, Veronika Schaffenroth
Figure caption:  O − C diagram (top) constructed from pulse timing measurements of roughly 0.2 day subsets of the 342 s pulsation period, along with residuals after subtracting the best-fitting sinusoid from the data (bottom).
Paper: Pulse Timing Discovery of a Three-day Companion to the Hot Subdwarf BPM 36430
Authors: Bryce A. Smith, Brad N. Barlow, Benjamin Rosenthal, J. J. Hermes, Veronika Schaffenroth
Figure caption: Radial-velocity curve of the sdBV primary in BPM 36430 (top). Residuals after subtracting the best-fitting sinusoid are also shown (bottom).
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: Schematic illustration of a Poynting-flux-dominated jet confined by the outer boundary wall made of the corona/wind region. The jet is accelerated outside the light cylinder and is denoted as the acceleration region (collimation and acceleration zone). In the highly magnetized funnel region, a stagnation surface is generated that separates the inflow and outflow regions. TT03 appropriately describes the poloidal velocity field of the jet flow in the outer region of the light cylinder (equivalent to the outer light surface) denoted as u  p (Ψ). The angular velocity of the magnetic field lines is denoted as Ω F . The TT03 model does not describe the interior of the light cylinder. We use cylindrical coordinates. The position coordinates of the outer boundary wall are denoted by the capital letters (R, Z). The value of the z coordinate of the light surface is different for each magnetic field line. The position where each magnetic field line intersects the light surface is the position of the light cylinder for each magnetic field line; thus the more distant the light surface from the inner magnetic field line, the farther away it is. We denote the z coordinate where the boundary wall (equivalent to the outermost magnetic field line) intersects the light surface as (R 0, Z 0).
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: Comparison of the model-predicted u  p  and the VLBI-measured u  p  as a function of the deprojected distance z from the black hole in units of r  g . The observation data points are adopted from Park et al. (2019b). The case in which parameter q = 1.3 is chosen for the boundary-wall shape is presented here. Although the TT03 model well reproduces the overall logarithmic acceleration of u  p , some offset remains at the inner region z ≲ 500 r  g . We also note that it is natural for the observed data and the model to have a gap below 106 r  g  as the region is beyond the domain of application of the model, where various dissipation processes are supposed to occur.
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: We show the Ψ dependence of u  p  by drawing the u  p  profile with Ψ = 0.1Ψ0, 0.2Ψ0,…,Ψ0. The fixed outer boundary wall has q = 1.3.
Paper: Implications from the Velocity Profile of the M87 Jet: A Possibility of a Slowly Rotating Black Hole Magnetosphere
Authors: Motoki Kino, Masaaki Takahashi, Tomohisa Kawashima, Jongho Park, Kazuhiro Hada, Hyunwook Ro, Yuzhu Cui, 玉竹 崔
Figure caption: Schematic illustration of the model overlaid on a stacked M87 image at 43 GHz (Y. Cui et al. 2022, in preparation). The TT03 model is applicable to the region outside the light cylinder. The model applicable range starts from z ≥ Z 0, at which the outer boundary wall and the light cylinder have intersection points, and it is located at ∼ (2–4) × 100r  g  from the central BH. As explained in the main body, the semi-parabolic boundary wall is determined by the jet width measurement by VLBI (Asada & Nakamura 2012; Hada et al. 2013).