adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Optical spectral comparison of SN 2022crv to other well-studied SESNe, including SNe Ib (SN 2007Y, iPTF13bvn, SN 2008D), SNe IIb (SN 1993J, SN 2008ax, SN 2011dh, SN 2009jf), and SNe Ic (SN 2007gr). The blue shaded areas mark the 6200 Å feature.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Nebular spectra of SN 2022crv compared with those of other SESNe. The phase is measured from the date of the V-band maximum brightness.
Paper: Very Extended Ionized Gas Discovered around NGC 1068 with the Circumgalactic Hα Spectrograph
Authors: Nicole Melso, David Schiminovich, Meghna Sitaram, Ignacio Cevallos-Aleman, Bárbara Cruvinel Santiago, Brian Smiley, Hwei Ru Ong
Figure caption: UV-optical diagnostic plots. Measurements for the ribbon, filament A, and the ring around NGC 1068 are shown as a square, triangle, and ring, respectively. Error bars represent the variation across each feature. We compare with existing measurements in the halos of NGC 253 and M82 (C. G. Hoopes et al. 2005) denoted by small gray open circles. We also compare with the FUV and Hα emission detected far into the halo of NGC 5128 around Centaurus A (S. G. Neff et al. 2015). Contours representing the Centaurus A weather ribbon measurement (1σ, 1.5σ, 2σ) are shown in blue. All measured values have been corrected for foreground Galactic reddening (see Section 3.3). Top left: ratio of Hα line flux to GALEX NUV flux density in units of angstrom as a function of Hα surface brightness. Top right: ratio of Hα line flux to GALEX FUV flux density in units of angstrom as a function of Hα surface brightness. Bottom left: diagnostic plot showing the ratio of Hα line flux to GALEX NUV flux density in units of angstrom vs. the unitless GALEX FUV-to-GALEX NUV flux density ratio. Bottom right: diagnostic plot showing the ratio of Hα line flux to GALEX FUV flux density in units of angstrom vs. the unitless GALEX FUV-to-GALEX NUV flux density ratio. We compare with models for photoionization, shocks, and shocks with photoionized precursors. Model details are discussed in Section 3.4.
Paper: Very Extended Ionized Gas Discovered around NGC 1068 with the Circumgalactic Hα Spectrograph
Authors: Nicole Melso, David Schiminovich, Meghna Sitaram, Ignacio Cevallos-Aleman, Bárbara Cruvinel Santiago, Brian Smiley, Hwei Ru Ong
Figure caption: CHαS spectral extraction and flux calibration for filament A and the ring. All panels have been rotated (∼15°) to align the hexagonally packed spectra along the Cartesian y-axis. The transformed coordinates can be compared directly with Figure 1. Left: relative velocity with respect to the systemic velocity of NGC 1068 (V sys = 1137 km s−1) from a Gaussian fit of each lenslet spectrum. Middle: velocity dispersion from the Gaussian fit to each lenslet spectrum. Right: surface brightness in each lenslet (2.″55 diameter, 5 arcsec2 solid angle) extracted with aperture photometry.
Paper: Characterization of the Western Pictor A Hotspot in Hard X-Rays with NuSTAR
Authors: Aamil Shaik, Eileen T. Meyer, Karthik Reddy, Sibasish Laha, Markos Georganopoulos
Figure caption: (Left): final combined NuSTAR image of Pictor A using FPMA and FPMB data from epochs 1 and 2. The images from each observation are aligned using cross correlations of the bright core. The images are then background-subtracted and exposure-corrected using background and exposure maps generated by nuskybgd and nuproducts, respectively. The individual flux images are then averaged and smoothed by a Gaussian at a factor of 2 pixels (4.″8) to produce the image above. The 50″ extraction region used for spectral analysis is encircled in magenta. The overlaid contours are taken from combined Chandra data. (Right): expanded image of the source region and western hotspot, again with Chandra contours overlaid. Unlike the high-resolution imaging of Chandra, NuSTAR is unable to resolve any structures or morphological features within the hotspot. The color bar below shows the image flux scale in units of ph s−1 cm−2.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Time–latitude plot of the radial field from the 2D model with Babcock–Leighton α for (a) v 0 = 4 m s−1 and (b) v 0 = 28 m s−1.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Time–latitude plot of the radial field from the 3D STABLE model with a single BMR for (a) v 0 = 4 m s−1, (b) v 0 = 8 m s−1, and (c) v 0 = 28 m s−1.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Time–latitude distribution of the surface radial magnetic field B r (in G) for stars with rotation periods of (a) 1 day, (b) 7 days, and (c) 25.38 days (solar value).
Paper: Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Artem Bohdan, Aaron Tran, Lorenzo Sironi, Lynn B. Wilson
Figure caption: Fourier power spectra of the shock precursor E ∥ for Runs A–E (top to bottom), measured in the downstream plasma’s rest frame. The left column is the (ω, k  x ) spectrum; the middle column is the (ω, k  y ) spectrum; and the right column is the (k  x , k  y ) spectrum. Each column is averaged over all k  y , k  x , and ω, respectively. The low-frequency, phase-standing precursor lies along ω/k  x  = v sh/r (left column, magenta line), where r is the shock’s density compression ratio; near the origin, the magenta line is not drawn, so that features of interest can be seen. A broad region of wave power has  k  along  B  and a downstream frame phase velocity ω/k that, when boosted to the upstream rest frame, is close to the upstream electron thermal speed v te0. To show this, the solid and dashed black lines plot ω = kv te0 − k  x  v 0 at propagation angles θ = 65° and 45°, respectively, measured counterclockwise from ﹩+\hat{{\boldsymbol{x}}}﹩ (i.e., ﹩\omega ={k}_{x}{v}_{\mathrm{te}0}/\cos \theta -{k}_{x}{v}_{0}﹩ (left column) and ﹩\omega ={k}_{y}{v}_{\mathrm{te}0}/\sin \theta -{k}_{y}{v}_{0}/\tan \theta ﹩ (middle column)). The θ angles bracket the range of  B  orientations within precursor wave troughs. The white circle (right column) is the 50% damping length induced by PIC current filtering (Section 2.1).
Paper: Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Artem Bohdan, Aaron Tran, Lorenzo Sironi, Lynn B. Wilson
Figure caption: Evolution of the electron acoustic mode ﹩{k}_{\max }﹩ (black solid line) from its most unstable wavenumber to a lower-k saturated state, and the peak power (red dashed line) in the reference PBCS.
Paper: Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Artem Bohdan, Aaron Tran, Lorenzo Sironi, Lynn B. Wilson
Figure caption: The parallel electric field maps at the maximum power of EAWs (left panel; ω pe t 1 = 47.5) and at the late stage of evolution (right panel; ω pe t 2 = 117.5) in the reference PBCS.
Paper: Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Artem Bohdan, Aaron Tran, Lorenzo Sironi, Lynn B. Wilson
Figure caption: Top panels: the growth rate of the EAWs for the near precursor and shock ramp parameters. Bottom panel: wavelength of the most unstable electron acoustic mode normalized to the electron skin depth (blue asterisks) and the Debye length (red asterisks). The faded red and blue circles show results from the shock simulations (also shown in Figure 7).
Paper: Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Artem Bohdan, Aaron Tran, Lorenzo Sironi, Lynn B. Wilson
Figure caption: Evolution of rms electric field fluctuation strength, ﹩| E| =\sqrt{\langle {E}^{2}\rangle }﹩, in the reference PBCS. The dashed–dotted line is the prediction of the linear dispersion analysis, ﹩{{\rm{\Gamma }}}_{{\rm{\max }}}/{\omega }_{\mathrm{pe}}=0.2﹩.
Paper: Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Artem Bohdan, Aaron Tran, Lorenzo Sironi, Lynn B. Wilson
Figure caption: Parallel electric field structure in the “Near Precursor” region for Runs A–E (left to right) at ﹩t=8.50{{\rm{\Omega }}}_{{\rm{i}}}^{-1}﹩. Each column of three panels shows one simulation. Within each column, the 2D image shows E ∥/E 0 with the same color map range as Figure 2 and the horizontal x-axis in units of the ion-scale precursor wavelength λ (the precursor’s magnetic minimum is at x = λ/4). Right of each 2D image, a plot of E ∥(y) (blue curve) shows the typical amplitude of ESWs and numerical noise at x = 3λ/8 (the dashed black line in the 2D image). Below each 2D image, the mean energy density ﹩\int {E}_{\parallel }^{2}(x,y)dy﹩ is plotted as a function of x (blue curve).
Paper: Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Artem Bohdan, Aaron Tran, Lorenzo Sironi, Lynn B. Wilson
Figure caption: The Fourier power spectrum of the electric field parallel to the magnetic field in the reference PBCS (black solid line) compared with the theoretical prediction (red dashed line).
Paper: Electrostatic Waves and Electron Holes in Simulations of Low-Mach Quasi-perpendicular Shocks
Authors: Artem Bohdan, Aaron Tran, Lorenzo Sironi, Lynn B. Wilson
Figure caption: The long-term evolution of the electric field in the reference PBCS and two runs with v dr multiplied by 0.5 and 0.25. These PBCSs mimic shock conditions from Runs A, C, and E.
Paper: Spectropolarimetry of Fraunhofer Lines in Local Upper Solar Atmosphere
Authors: Z. Q. Qu, L. Chang, G. T. Dun, X. M. Cheng, C. Fang, Z. Xu, D. Yuan, L. H. Deng, X. Y. Zhang
Figure caption: SE205-1. Top panel: the raw spectral image. Lower panels: the intensity I and fractional linear polarization Q/I profiles obtained in the panels below from the polarization demodulation after spatial binning over P1–P10, P11–P25, and all of the volumes (P1–P25) of the FOV respectively. Note that the polarizations of F-corona, E-corona, and K-corona are given.
Paper: Spectropolarimetry of Fraunhofer Lines in Local Upper Solar Atmosphere
Authors: Z. Q. Qu, L. Chang, G. T. Dun, X. M. Cheng, C. Fang, Z. Xu, D. Yuan, L. H. Deng, X. Y. Zhang
Figure caption: SE204-3. Top panel: the raw spectral image. Lower panels: the intensity I and fractional linear polarization Q/I profiles obtained from the polarization demodulation after spatial binning over P1–P10, P11–P25, and all of the volumes (P1–P25) of the FOV respectively. The green coronal line is the broadest line at 530.3 nm.
Paper: Spectropolarimetry of Fraunhofer Lines in Local Upper Solar Atmosphere
Authors: Z. Q. Qu, L. Chang, G. T. Dun, X. M. Cheng, C. Fang, Z. Xu, D. Yuan, L. H. Deng, X. Y. Zhang
Figure caption: SE196-4. Top panel: the raw spectral image. Lower panels: the intensity I and fractional linear polarization Q/I profiles obtained from polarization demodulation after spatial binning over point one to point fifteen (P1–P15), P16–P25, and all of the points (P1–P25) of the FOV respectively.
Paper: Spectropolarimetry of Fraunhofer Lines in Local Upper Solar Atmosphere
Authors: Z. Q. Qu, L. Chang, G. T. Dun, X. M. Cheng, C. Fang, Z. Xu, D. Yuan, L. H. Deng, X. Y. Zhang
Figure caption: The intensity I profiles respectively of P14, P16, P20, and P22 of SE204-3, for illustrating the relative line center shifts due to the Doppler effect. Note a cosmic event causing a strong emission at 520.9 nm at P22. The intensities of P20 are artificially added with 250 cts, and intensities of both P16 and P14 are added respectively with 600 cts and 800 cts in order to separate these four profiles within one panel.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: Overview of the proposed MEASNet and its blocks. (a) MEASNet. (b) ATCB. (c) STB. (d) Gate recurrent unit.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: Distribution of the difference between MEASNet predictions and GALAH labels as a function of S/N. The x-axis is the average of the r-band and g-band S/N, and the y-axis is the difference, which is defined as MEASNet predictions minus GALAH labels. The color represents the density of samples. Deep red points mark the μ for bins at 100 intervals, and the length of the deep red whiskers signifies the σ within each bin.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: Cross-validations of the MEASNet prediction derived using the LAMOST-GALAH training set. Each subfigure plots labeled values on the x-axis against predicted values on the y-axis, with points colored by data density. The red dashed line represents the 1:1 line, where predictions match the actual values. Ideally, sample points should closely align with this line. The numerals in the lower right corner of each subfigure indicate the number of test set samples for each element.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: The original LAMOST spectrum (top panel), and its normalized spectrum (bottom panel).
Paper: Radio Scrutiny of the X-Ray-weak Tail of Low-mass Active Galactic Nuclei: A Novel Signature of High-Eddington Accretion?
Authors: Jeremiah D. Paul, Richard M. Plotkin, W. N. Brandt, Christopher H. Ellis, Elena Gallo, Jenny E. Greene, Luis C. Ho, Amy E. Kimball, Daryl Haggard
Figure caption: Spectral fit for the GH 69 Chandra observation (see Appendix A.2.2). Residuals are displayed as ΔC/∣ΔC∣1/2, where C is the Cash statistic.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: Distribution of T eff and ﹩\mathrm{log}\,g﹩ for the reference set colored by [Fe/H].
Paper: Detection of Dimethyl Ether in the Central Region of the MWC 480 Protoplanetary Disk
Authors: Yoshihide Yamato, Yuri Aikawa, Viviana V. Guzmán, Kenji Furuya, Shota Notsu, Gianni Cataldi, Karin I. Öberg, Chunhua Qi, Charles J. Law, Jane Huang, Richard Teague, Romane Le Gal
Figure caption: Summary of the observations toward the MWC 480 disk. Top: 1.03 mm continuum image (left) and velocity-integrated intensity maps of (tentatively) detected COMs, CH3OCH3, and CH3OCHO (others). The peak S/Ns of the right three maps are 5.4, 12, and 6.0, respectively. The white ellipse in the lower left corner indicates the synthesized beam. A scale bar of 50 au is shown in the lower right corner. Middle: spectra extracted in a circular aperture with 0.″6 diameter toward the disk center (gray), overlaid with the best-fit spectral model for CH3OCH3  (blue), CH3OCHO (orange), and the sum of both (black). The semitransparent error bars represent the associated 1σ uncertainties. The frequency ranges removed from the fit due to the atmospheric absorption or contamination from other molecular lines are shaded in gray. Bottom: zoom-in view of the middle panel in the vicinity of the (tentatively) detected features, but with the spectral axis in velocity with respect to a reference frequency of 299.11170 GHz (left), 299.89209 GHz (middle), and 300.05338 GHz (right), respectively. The vertical line segments at the bottoms of the panels indicate the center and the relative strength (at 200 K) of each transition.
Paper: Detection of Dimethyl Ether in the Central Region of the MWC 480 Protoplanetary Disk
Authors: Yoshihide Yamato, Yuri Aikawa, Viviana V. Guzmán, Kenji Furuya, Shota Notsu, Gianni Cataldi, Karin I. Öberg, Chunhua Qi, Charles J. Law, Jane Huang, Richard Teague, Romane Le Gal
Figure caption: Comparison of the column density ratios of CH3OCH3 and CH3OCHO relative to CH3OH in three disks: HD 100546 (Booth et al. 2024a), Oph IRS 48 (Booth et al. 2024b), and MWC 480 (this work). The upward and downward triangles indicate lower and upper limits, respectively. Given the tentative detection (see Section 3.2), the value of CH3OCHO in MWC 480 is plotted with transparency. The shaded region indicates the typical range of protostellar values measured by extensive line surveys (PILS—Jørgensen et al. 2016; CALYPSO—Belloche et al. 2020; PEACHES—Yang et al. 2021).
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: Three distributions are presented in the [Fe/H]–[X/Fe] space: all barium candidates, dwarf and subgiant barium candidates (﹩\mathrm{log}\,g﹩ ≥ 3.5 dex), and giant barium candidates (﹩\mathrm{log}\,g﹩ < 3.5 dex). The x-axis represents [Fe/H] from LAMOST, while the y-axis shows MEASNet predictions. Gray points indicate barium candidates with [Ba/Fe] values between 0.25 and 1.0 dex. The color represents the T eff distribution of samples.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: The relationship between GALAH labels and the uncertainty of MEASNet with box plots. In each box, the orange line signifies the median uncertainty. The first (Q1) and third (Q3) quartiles are represented by the bottom and top edges of the box, respectively. The interquartile range (IQR) is calculated as IQR = Q3 − Q1. The whiskers, or lines extending from the box, denote the range within which most values fall, specifically up to Q3 + 1.5 × IQR for the upper whisker and down to Q1 − 1.5 × IQR for the lower whisker.
Paper: Detection of Dimethyl Ether in the Central Region of the MWC 480 Protoplanetary Disk
Authors: Yoshihide Yamato, Yuri Aikawa, Viviana V. Guzmán, Kenji Furuya, Shota Notsu, Gianni Cataldi, Karin I. Öberg, Chunhua Qi, Charles J. Law, Jane Huang, Richard Teague, Romane Le Gal
Figure caption: Matched filter responses. The horizontal dotted line marks 5σ. The relative intensities of the covered lines at 200 K are shown by the vertical segments for CH3OCH3 (blue), CH3OCHO (orange), CH3OH (red), and CH3CHO (green). A cluster of CH3OCH3 lines at ∼299.89 GHz exhibits a ∼17σ response, while the tentative features at ∼299.12 GHz and ∼300.06 GHz show ∼5σ–6σ responses.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: Distribution of the difference between MEASNet predictions and GALAH labels as a function of [Fe/H]. The x-axis is the [Fe/H] measured by LAMOST, and the y-axis is the difference, which is defined as MEASNet predictions minus GALAH labels. The color represents the density of samples. Deep red points mark the μ for bins at 0.25 dex intervals, and the length of the deep red whiskers signifies the σ within each bin.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: Focus regions of MEASNet during abundance prediction. The top 50 focus regions, categorized into intervals of 20 Å, are displayed. A color gradient from deep red to light red is used to indicate the level of attention in these regions, from high to low.
Paper: MEASNet. I. A Model for Barium Star Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey
Authors: Shengjun Song, Xiaoming Kong, Yude Bu, Zhenping Yi, Meng Liu
Figure caption: Spectra around the absorption lines of different elements under two sets of atmospheric parameters. In each graph, the black, red, green, and blue spectral curves represent increasing levels of element abundance.
Paper: It’s a Breeze: The Circumgalactic Medium of a Dwarf Galaxy Is Easy to Strip
Authors: Jingyao Zhu, Stephanie Tonnesen, Greg L. Bryan, Mary E. Putman
Figure caption: Dwarf satellite gas mass and orbital ram pressure time evolution. Top panel: gas mass within the CGM region, defined as r disk,0 < r < 1.5r vir (the initial gas disk radius to 1.5 times the virial radius; see Section 2). The lines show the two wind runs and iso control with satellite CGM. Middle panel: gas mass within the ISM region, defined as r ≤ r disk,0, showing the runs with CGM as solid lines and those without CGM as dashed–dotted lines in the same color. Bottom panel: ram pressure of the MW-w and weak-w orbits (host R 200 to R peri and back to R 200; Section 2.2). The initial ∼550 Myr before the first shock reaches the central galaxy is shaded in gray.
Paper: It’s a Breeze: The Circumgalactic Medium of a Dwarf Galaxy Is Easy to Strip
Authors: Jingyao Zhu, Stephanie Tonnesen, Greg L. Bryan, Mary E. Putman
Figure caption: Gas stripping morphology of the MW-w simulation (Table 3). The different panels show the gas surface density (Σgas, top row) and the ISM and CGM tracer fractions (middle and bottom rows; color tracers described in Section 2.3) at four example snapshots (columns left to right). The Σgas panels are projected face-on (along the z-axis: aligned with the disk rotation axis and 45°-angled with the wind), while the two color tracers are projected edge-on (along the x-axis) to better show global morphology under the 45° wind. Most of the CGM is quickly removed before effective ISM stripping takes place (third column), as elaborated in Section 4.1.