adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: N/O as a function of C/O (bottom right). The symbols are the same as in Figure 6, while the blue dashed, green solid, and yellow dashed–dotted lines illustrate chemical evolution models of Wolf–Rayet (WR) stars, supermassive stars (SMSs), and tidal disruption events (TDEs), respectively, where most of massive stars are assumed to undergo the direct collapse (Watanabe et al. 2023; K. Watanabe et al. 2023, in preparation).
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: N/O as a function of absolute UV magnitude M UV (left) and S/N ratio of Hδ (right). The symbols are basically the same as those in the top right panel of Figure 6, but our sample galaxies with S/N(H δ) < 3 are shown by the gray arrows only in the right panel. The white circle represents the N/O upper limit derived from the stacked spectrum of our sample galaxies. The black dashed line is the solar abundance.
Paper: JWST Identification of Extremely Low C/N Galaxies with [N/O] ≳ 0.5 at z ∼ 6–10 Evidencing the Early CNO-cycle Enrichment and a Connection with Globular Cluster Formation
Authors: Yuki Isobe, Masami Ouchi, Nozomu Tominaga, Kuria Watanabe, Kimihiko Nakajima, Hiroya Umeda, Hidenobu Yajima, Yuichi Harikane, Hajime Fukushima, Yi Xu, Yoshiaki Ono, Yechi Zhang
Figure caption: Ar/O and S/O as a function of metallicity. The symbols are the same as those in Figure 9, while we add Watanabe et al. (2023)'s chemical evolution models of HNe with different metallicities (green) and isochrones (light green).
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Top: The observed velocity evolution of the Si II PVF and HVF of SN 2021aefx is compared to those of other normal Type Ia SNe, those of the Ca II NIR triplet PVF and HVF (Appendix) and the C II feature of SN 2021aefx, and the best-fit β = −0.22 power law (solid magenta lines with dashed extrapolations). The x-axis represents time in days since the fitted explosion epoch (=﹩{t}_{\exp }﹩) obtained using this power law. The gray dashed lines show the t −0.22 evolution of the pre-peak Si II velocities in the other SNe. Bottom: ﹩{\chi }_{{\rm{R}}}^{2}﹩ of fitting t −β  power laws to the Si II PVF velocity evolution of SN 2021aefx before B-band maximum and the Si II HVF velocity evolution before the onset of its HVF plateau (∼3.6 rest-frame days post-explosion). Note that β = −0.22 is the theoretically expected photospheric evolution for Type Ia SN ejecta.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Left: Spectra of SN 2021aefx (black) in the vicinity of the Si II λ6355 Å feature compared to multicomponent Gaussian fits (yellow dotted curve) with PVF (blue solid curves), HVF (cyan dashed curves), and C II (magenta dashed curves) components at ten evolutionary phases, as labeled on the bottom left in rest-frame days since B-band maximum. Rows (1)–(3) are during the early PVF and HVF decline, (4)–(6) span the HVF plateau (see Figure 7), (7) is the last epoch when the HVF is detected, (8) is at B-band maximum, (9) has the largest ﹩{\chi }_{{\rm{R}}}^{2}﹩ (see Table 4), and (10) is the last phase when the Si II λ6355 Å feature is detected. The red shaded line is the estimated continuum of the feature, while the vertical dotted lines indicate the fitted minima of the correspondingly colored Gaussian components. Right: The same spectra and fits, but the wavelength axis is converted to velocity in the rest frame of the fitted PVF minima at each phase (middle blue vertical dotted line at 0 km s−1). The cyan vertical dotted line with shaded region represents the mean and 1σ velocity of the fitted HVF minima in this frame. The blue vertical dotted lines flanking the PVF and HVF are the expected positions of the photospheric-velocity Si II λ5972 Å and C II λ6580 Å features, as labeled at the top of the first panel. C II λ6580 Å is detected in only a few spectra (see Table 4) near this photospheric velocity.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Left: The early (< − 10 days) UBVi-band light curves of SN 2021aefx are compared to the models (1) pure power law (green) obtained by fitting the optical (BVi-band) light curves over an extensive set of fit intervals between − 20 and − 10 days; and (2) power law + Gaussian fitted to the light curves over the entire interval. The vertical green and blue dotted lines indicate the onsets of the power-law components for the correspondingly colored models. The inset zooms in on the excess emission in the first ∼3 days. Right: The early light curves compared to the same models, with the power laws of the models subtracted. The green data points represent the result of subtracting the pure power law, which leaves residuals between the data points and the model (green solid curve). The blue data points represent that of subtracting the power-law component of the power-law + Gaussian fit, which leaves residuals that are captured by the Gaussian component. The onset of the power-law component of the power law + Gaussian fit (vertical blue dotted line) is used to estimate t PL (Table 3).
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Top left: Branch et al. (2006) classification diagram comparing the pseudo-equivalent widths of Si II lines of SN 2021aefx from a spectrum near B-band maximum (−0.5 day; orange star) with those from a population of Type Ia SNe (Blondin et al. 2012). The colored symbols represent events from the four main subtypes of Type Ia SNe: CN (blue circles), BL (cyan squares), shallow-silicon (red triangles), and cool (green diamonds). Note that CN and BL are both subsets of normal Type Ia SNe, while shallow-silicon and cool are considered peculiar. Bottom left: Wang et al. (2009) classification diagram comparing the S II λ6355 Å equivalent width and Doppler velocity of SN 2021aefx from near B-band maximum (orange star) with those of the same population of Type Ia SNe from the top left panel. The NV, HV, 91T-like, and 91bg-like subtypes represented by the colored symbols approximately correspond to the CN, BL, shallow-silicon, and cool subtypes respectively. Top right: Comparison of the M  B  (peak) and ΔM 15(B) of SN 2021aefx (orange star) with those of other Type Ia SNe (gray crosses; Burns et al. 2018). The average values for the four main subtypes of Type Ia SNe are represented by their correspondingly colored symbols, while the magenta pentagon represents the average for the extremely slow-declining and overluminous events once thought be from super-Chandrasekhar-mass explosions (Parrent et al. 2014) called “03fg/09dc-like” (Taubenberger et al. 2019; Ashall et al. 2020). Bottom right: comparison of the ΔM 15(B) and peak Si II velocity of SN 2021aefx (orange star) with a population of other Type Ia SNe (Parrent et al. 2014) with colored symbols representing the same subtypes as in the top right panel.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: The BVi (blue, green, and red data points, respectively) light curves of SN 2021aefx are compared to those of normal Type Ia SNe 2018aoz (Ni et al. 2022, 2023), 2011fe (Guillochon et al. 2017), 2018oh (Dimitriadis et al. 2019), and 2017cbv (Hosseinzadeh et al. 2017) as well as the peculiar Type Ia SN MUSSES1604D (Jiang et al. 2017) in their nearest-to-V bands centered at maximum light. The errorbars represent the 1σ uncertainty level, and inverted arrows are 3σ detection limits in this figure and all of the following. The inset shows the early light curves within 5 days of their t PL (often called epoch of “first light”), where excess emission has previously been identified in some Type Ia SNe (Hosseinzadeh et al. 2017; Stritzinger et al. 2018; Dimitriadis et al. 2019), normalized to their fluxes at 5 days. SN 2018oh, SN 2017cbv, and MUSSES1604D each show excess emission between 1 and 5 days, whereas SNe 2011fe and 2018aoz show a typical power-law-like rise. The power-law rise of SN 2021aefx based on fitting a power-law + Gaussian model (see Figure 4) is shown with blue, green, and red curves. The early excess emission in SN 2021aefx, indicated with the magenta vertical dashed line, is clearly different from those of other SNe.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Spectra of SN 2021aefx (black) from −16.7, −15.7, and −0.5 days (as labeled) since B-band maximum in rest frame are compared to those of other normal Type Ia SNe. The first two spectra were obtained by SALT during the excess emission phase—i.e., prior to 1.75 days since t PL (see Section 3.1)—while the third is our spectrum from near B-band maximum. The near-peak-spectrum is translated downwards (gray) by subtracting a constant value to compare with those of five other normal Type Ia SNe: core-normal events (blue) SNe 1994D (Meikle et al. 1996) and 2011fe (Parrent et al. 2012), broad-line events (cyan) SNe 1981B (Branch et al. 1983) and 2009ig (Foley et al. 2012), and intermediate event SN 2018aoz (orange; Ni et al. 2023). Notable spectral features from the excess emission phase and near-peak phase are marked above the spectra from each phase, respectively. The spectrum of SN 2021aefx appears to resemble that of SN 2009ig during the excess emission phase prior to ∼ − 15 days, although it becomes more similar to SN 2018aoz near B-band maximum.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: The early B − V color of SN 2021aefx is compared to those of other Type Ia SNe showing that SN 2021aefx undergoes a unique redward color evolution over the first ∼2 days that is faster than that of MUSSES1604D and slower than that of SN 2018aoz before evolving bluewards, falling in line with early red events including SNe 2018aoz and 2011fe (Stritzinger et al. 2018).
Paper: Multiwavelength Study of Dark Globule DC 314.8–5.1: Point-source Identification and Diffuse Emission Characterization
Authors: E. Kosmaczewski, Ł Stawarz, C. C. Cheung, A. Bamba, A. Karska, W. R. M. Rocha
Figure caption: Top: SED of the DC 314.8–5.1 system, based on observations with Planck (filled black circles), IRAS (red crosses), and WISE (open red circles). Dark red solid and dashed curves represent modified blackbody models for the emission of cold (14 K) and warm (160 K) gas within or on the surface of the cloud, respectively; the black solid curve denotes the superposition of the two. Bottom: SED of HD 130079 from ground-based telescopes and the Gaia survey (small blue stars), WISE (open red circles), and finally with the Swift UVOT (big blue star). The dark blue dotted–dashed curve corresponds to the intrinsic emission of the field star HD 130079, modeled as a blackbody with the temperature 10,500 K and a total luminosity of 3 × 1035 erg s−1; the dark blue solid curve illustrates this intrinsic emission subjected to the interstellar reddening. See Section 4 for a description.
Paper: Multiwavelength Study of Dark Globule DC 314.8–5.1: Point-source Identification and Diffuse Emission Characterization
Authors: E. Kosmaczewski, Ł Stawarz, C. C. Cheung, A. Bamba, A. Karska, W. R. M. Rocha
Figure caption: DC 314.8–5.1 region as seen at different wavelengths. Top left: Spitzer MIPS 24 μm log-scaled intensity mosaic map; top right: Spitzer IRAC 5.8 μm log-scaled intensity mosaic map; bottom left: DSS red linear scaled image (700 nm); bottom right: Swift UVOT M2–2250 Å band log-scaled map. In each panel, the white dashed ellipse denotes the globule with the central position marked by a white “×.” The green ellipses mark UVOT-detected sources with HD 130079 marked on the left and TYC 9015-926-1 marked near the northern boundary of the globule. “C1” marks the YSO candidate identified by Whittet (2007). “C2” and “C3” mark the potential YSO candidates identified in this work. The X-ray source detected with Swift-XRT is indicated by “S” with a cross.
Paper: Multiwavelength Study of Dark Globule DC 314.8–5.1: Point-source Identification and Diffuse Emission Characterization
Authors: E. Kosmaczewski, Ł Stawarz, C. C. Cheung, A. Bamba, A. Karska, W. R. M. Rocha
Figure caption: DC 314.8–5.1 as seen by Planck at 353 GHz (left panel) and IRAS at 60 μm (right panel). The white dashed ellipse (with radii of ﹩\sim 7^{\prime} \times 5^{\prime} ﹩) denotes the globule, with the central position marked by a black “×.” The star HD 130079 is marked with a black open circle to the east of the cloud center.
Paper: Multiwavelength Study of Dark Globule DC 314.8–5.1: Point-source Identification and Diffuse Emission Characterization
Authors: E. Kosmaczewski, Ł Stawarz, C. C. Cheung, A. Bamba, A. Karska, W. R. M. Rocha
Figure caption: Spitzer IRAC-band maps of the DC 314.8–5.1 region. Top left: channel 1 at 3.6 μm; top right: channel 2 at 4.5 μm; bottom left: channel 3 at 5.8 μm; bottom right: channel 4 at 8.0 μm. The white dashed ellipse marks the optical extent of DC 314.8–5.1. The color bar is set with a minimum of zero and a maximum value of 200 MJy sr−1 on a log scale. The field star HD 130079 is marked in the left of each image, “C1” marks the YSO candidate identified by Whittet (2007), and “C2” marks the YSO candidate identified in this work.
Paper: Multiwavelength Study of Dark Globule DC 314.8–5.1: Point-source Identification and Diffuse Emission Characterization
Authors: E. Kosmaczewski, Ł Stawarz, C. C. Cheung, A. Bamba, A. Karska, W. R. M. Rocha
Figure caption: Top: full-band 0.3–10 keV Swift-XRT image of the DC 314.8–5.1 region, smoothed with a Gaussian of radius 6 pixels. The field star HD 130079 is marked in the left of each image. “C1” marks the YSO candidate identified by Whittet (2007). “C2” and “C3” mark the potential YSO candidates identified in this work. The color bar indicates the linear intensity scale for the smoothed (averaged) counts. Bottom left: soft band 0.3–2.0 keV; bottom right: hard band 2–10 keV.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The transmission spectrum atmospheric effective altitude is plotted against wavelength between 0.2 and 11 μm for the P19 PI (orange), P19 10% PAL (brown), P19 1% PAL (yellow), and P19 0.1% PAL (red) simulations, and the W21 PI (light blue), W21 10% PAL (blue), W21 1% PAL (lilac), and W21 0.1% PAL (gray) simulations. The non–tidally locked cases are excluded for clarity, but show little differences compared to the equivalent tidally locked case. The transit depth, in terms of contrast with respect to the star, is indicated on the right vertical axis in units of ppm. The spectra are binned to a spectral resolving power of R = 250. Spectral features are indicated in gray. The wavelength range of the proposed Habitable Worlds Observatory (HWO; blue shaded region), and that of the JWST NIRSpec instrument (yellow shaded region), are shown. They overlap in the green shaded region. The wavelength range of the JWST MIRI instrument is indicated in the magenta shaded region. The wavelength spacing between 0.2 and 1 μm is changed between 1 and 11 μm in order to show the UV and visible regions clearly. The black bar represents the uncertainty that would be present on a measurement that has reached the noise floor of the instrument, where the noise floor is indicated as 5 ppm. Note this error bar is an estimate of the performance of the telescope and does not indicate a measurement.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The surface temperatures in kelvin are shown for the P19 (left column) and W21 (right column) PI, noTL, 10% PAL, 1% PAL, and 0.1% PAL scenarios. In the tidally locked cases, a relatively warm region exists around the substellar point, which receives constant irradiation. The substellar point for the tidally locked cases is at 180° longitude and 0° latitude (in the center of each Robinson projection). In the P19 and W21 noTL cases, the substellar point moves because there is a diurnal cycle. These simulations have the coldest surface temperatures (171 and 170 K, respectively), but the smallest range in surface temperatures.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The left panel shows the PSG simulations of planetary spectral radiance from emission spectra focused on the 4.71 μm O3 feature (which overlaps with a CO2 feature, both shown by the gray shaded regions) for the P19 PI (orange), P19 10% PAL (brown), P19 1% PAL (yellow), and P19 0.1% PAL (red) simulations, and the W21 PI (light blue), W21 noTL (black), W21 10% PAL (blue), W21 1% PAL (lilac), and W21 0.1% PAL (gray) simulations. The right panel shows the same for the 9.6 μm O3 feature, shown by the gray shaded region. Telescopes and their instruments which may be able to probe atmospheres in the infrared include: the Extremely Large Telescope (ELT; Brandl et al. 2021) METIS instrument, the Large Interferometer for Exoplanets (LIFE; Konrad et al. 2022), and the JWST (Morley et al. 2017) NIRSpec and MIRI instruments.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The oxygen (O2) concentration is shown against the ozone (O3) column in each simulation (orange for P19 scenarios and blue for W21 scenarios). The “error bar” lines show the range between the minimum and maximum O3 columns in each simulation. The circular dots show the mean O3 columns. The O3 columns simulated by WACCM6 for Earth, from Cooke et al. (2022), are shown in black for comparison.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The high cloud fraction, where high clouds are specified as clouds at pressures below 400 hPa, is shown for the PI and 0.1% PAL simulations in the P19 (left) and W21 (right) scenarios. Blue shows low cloud fraction, while white shows large amounts of cloud coverage. Clouds provide a net warming in the tidally locked scenarios.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The H2O column, given in terms of kgm−2, is shown for the PI and 0.1% PAL simulations in the P19 (left) and W21 (right) scenarios. White shows a relatively low H2O column, while blue shows relatively large amounts of H2O column. For reference, Earth’s H2O column reaches a peak of about 50 kg m−2.
Paper: Electromagnetic Characterization of the LISA Verification Binary ZTF J0526+5934
Authors: Alekzander Kosakowski, Thomas Kupfer, P. Bergeron, Tyson B. Littenberg
Figure caption: Left: best-fitting LCURVE models overplotted onto the phase-folded McDonald 2.1 m telescope ﹩g^{\prime} ﹩-band (top), ﹩r^{\prime} ﹩-band (middle), and ﹩i^{\prime} ﹩-band (bottom) light curves. Right: parameter distributions for the mass ratio (q = M 2/M 1 < 1.0), orbital inclination (i), volumetric scaled stellar radius (r 2,vol = R 2,vol/a), and stellar mass M 2. We mark the upper and lower 1σ error values as the 84.13 and 15.97 percentiles to each parameter distribution, respectively.
Paper: Electromagnetic Characterization of the LISA Verification Binary ZTF J0526+5934
Authors: Alekzander Kosakowski, Thomas Kupfer, P. Bergeron, Tyson B. Littenberg
Figure caption: Left: ZTF DR16 light curve of J0526+5934 (top), its Lomb–Scargle power spectrum (middle), and phase-folded ZTF DR16 light curve (bottom). Data points are colored based on the filter used. Green data points represent ZTF_g; red data points represent ZTF_r. Right: Gaia DR3 color–magnitude diagram. The location of J0526+5934 is marked with a red symbol.
Paper: Electromagnetic Characterization of the LISA Verification Binary ZTF J0526+5934
Authors: Alekzander Kosakowski, Thomas Kupfer, P. Bergeron, Tyson B. Littenberg
Figure caption: Best-fitting exposure-averaged integrated sine curve (red dashed line; EXPTIME = 120 s) to the Keck LRIS radial velocity measurements of ZTF J0526+5934 (black points).
Paper: Electromagnetic Characterization of the LISA Verification Binary ZTF J0526+5934
Authors: Alekzander Kosakowski, Thomas Kupfer, P. Bergeron, Tyson B. Littenberg
Figure caption: Best-fitting model atmosphere to the coadded optical spectrum of ZTF J0526+5934.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three-dimensional plot of the evolution of the smoothed magnetic field component in the plane orthogonal to the shock normal  B  ⊥ = B  l   l   a  + B  m   m   a , as observed during the Venusian bow shock crossing on 2011 July 26. The distance scale represents the distance from the shock (crossing time 03:56:27) along the shock normal direction.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three components and the magnitude of the magnetic field in the shock coordinate system, based on  n  MV as observed during the Venusian bow shock crossing on 2011 July 26. The gray shaded region marks the shock transition region.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three components and the magnitude of the magnetic field in the shock coordinate system, based on  n  MV as observed during the first Venusian bow shock crossing on 2011 December 15. The transition region is shaded in gray.