adsabs/AstroCLIMB huggingface dataset:
Paper: Observations of Twist, Current Helicity, and Writhe in the Magnetic Knots of δ-sunspots Consistent with the Kink Instability of a Highly Twisted Flux Rope
Authors: Peter J. Levens, Aimee A. Norton, Mark G. Linton, Kalman J. Knizhnik, Yang Liu
Figure caption: The continuum intensity, I  c  (left), radial magnetic field, B  r  (middle), and current helicity, H  r   c  (right) is shown for the three δ-spots with NOAA numbers 11158, 11267, and 11476. The time of observation, NOAA number, and northern (N) or southern (S) hemisphere are shown on the lower portion of the continuum intensity image. The red and yellow contours outline the positive and negative magnetic umbrae participating in the magnetic knot, respectively. The time shown for each AR corresponds to the time of maximum, total H  r   c  in the magnetic knot. Each image axis is in units of pixels with the length of 1 pixel being roughly 0.36 Mm on the surface of the Sun as per the Lambert cylindrical equal-area projection of these HMI data products. These data will be shown in higher resolution in subsequent figures but is shown here to provide context.
Paper: Observations of Twist, Current Helicity, and Writhe in the Magnetic Knots of δ-sunspots Consistent with the Kink Instability of a Highly Twisted Flux Rope
Authors: Peter J. Levens, Aimee A. Norton, Mark G. Linton, Kalman J. Knizhnik, Yang Liu
Figure caption: Histograms showing the distribution of pixels within each knot having certain values of current helicity, H  r   c , are shown for NOAA 11158, 11267, and 11476, from left to right, respectively, with corresponding dates and times of 2011.02.14_02:36:00, 2011.08.07_01:12:00, and 2012.05.07_13:12:00. Bins are 1 × 105 Mx2 cm−2 wide. A vertical dashed line is placed at the median pixel current helicity value within each knot.
Paper: Spectral Survey of a Hot Core with an Eruptive Accretion in S255IR NIRS3 (SHEA): The Discovery of Class I and II Millimeter Methanol Maser Transitions
Authors: Giseon Baek, Jeong-Eun Lee, Neal J. Evans, Tomoya Hirota, Yuri Aikawa, Ji-hyun Kang, Jungha Kim, Jes K. Jørgensen
Figure caption: Top panels: integrated intensity (left) and peak T b (right) maps of CH3OH 83,5–82,6A line overlaid with the 1.2 mm continuum map (contour). The intensity at the velocity range of −3.8 and 11.2 km s−1 is integrated with >5σ of rms noise. The contour levels for the continuum emission are 0.3, 0.7, 1.5, 3.5, 7.9, and 18.0 mJy beam−1. Bottom panels: the same maps as the top panels, but for CH3OH 61,5–52,4E line. The white cross in the peak T b map marks the region from which the line profiles in Figure 2 are extracted.
Paper: CUTE Reveals Escaping Metals in the Upper Atmosphere of the Ultrahot Jupiter WASP-189b
Authors: A. G. Sreejith, Kevin France, Luca Fossati, Tommi T. Koskinen, Arika Egan, P. Wilson Cauley, Patricio. E. Cubillos, S. Ambily, Chenliang Huang, Panayotis Lavvas, Brian T. Fleming, Jean-Michel Desert, Nicholas Nell, Pascal Petit, Aline Vidotto
Figure caption: NUV broadband light curve and transmission spectrum obtained from WASP-189b analysis. Top: broadband NUV light curve of WASP-189b for a 800 Å bin centered at 2900 Å. Middle: transmission spectrum at variable resolutions (black filled circles) with reference and best-fit models (light blue and pink, respectively). Bottom left: high-resolution models showing the variation of the ratio of planetary radius (R  p ) with optical planetary radius (R opt) as a function of wavelength. Bottom right: T–P profiles used to generate the transmission spectrum (reference model in light blue and the best-fit model in pink).
Paper: Spectral Survey of a Hot Core with an Eruptive Accretion in S255IR NIRS3 (SHEA): The Discovery of Class I and II Millimeter Methanol Maser Transitions
Authors: Giseon Baek, Jeong-Eun Lee, Neal J. Evans, Tomoya Hirota, Yuri Aikawa, Ji-hyun Kang, Jungha Kim, Jes K. Jørgensen
Figure caption: The intensity-weighted velocity maps (colored image) and the velocity distribution of the peak intensity positions (symbol) of CH3OH transitions. The contour is the 1.2 mm continuum map, as in Figure 1. The intensity-weighted velocity map of the first transition in the legend (the strongest emission) is shown in each panel. The color image has lightened with α = 0.8 (0: transparent, 1: opaque). The symbol denotes the location of the emission peak in each channel. The color of the symbol shows the velocity at the peak intensity position, identical to the color image scale. Symbol size is proportional to the intensity. P and A denote the 6.7 GHz class II CH3OH maser clusters observed before and after the accretion burst of S255IR NIRS3 (Moscadelli et al. 2017; Szymczak et al. 2018) Top: transitions that class II CH3OH maser is predicted by the model (Table 1). Middle: class II maser candidate transitions that behave similarly to that presented in the top panel, without model prediction. Bottom: thermal transitions.
Paper: Spectral Survey of a Hot Core with an Eruptive Accretion in S255IR NIRS3 (SHEA): The Discovery of Class I and II Millimeter Methanol Maser Transitions
Authors: Giseon Baek, Jeong-Eun Lee, Neal J. Evans, Tomoya Hirota, Yuri Aikawa, Ji-hyun Kang, Jungha Kim, Jes K. Jørgensen
Figure caption: Top panel: excitation diagram of CH3OH. In a range of 238–275 GHz, emission lines with A  ij  < −4.25 are adopted. Bottom panels: observed (gray) and model (green) spectra of CH3OH in S255IR NIRS3 (the position in Figure 1(d) marked with a cross).
Paper: AT 2022aedm and a New Class of Luminous, Fast-cooling Transients in Elliptical Galaxies
Authors: M. Nicholl, S. Srivastav, M. D. Fulton, S. Gomez, M. E. Huber, S. R. Oates, P. Ramsden, L. Rhodes, S. J. Smartt, K. W. Smith, A. Aamer, J. P. Anderson, F. E. Bauer, E. Berger, T. de Boer, K. C. Chambers, P. Charalampopoulos, T.-W. Chen, R. P. Fender, M. Fraser, H. Gao, D. A. Green, L. Galbany, B. P. Gompertz, M. Gromadzki, C. P. Gutiérrez, D. A. Howell, C. Inserra, P. G. Jonker, M. Kopsacheili, T. B. Lowe, E. A. Magnier, C. McCully, S. L. McGee, T. Moore, T. E. Müller-Bravo, M. Newsome, E. Padilla Gonzalez, C. Pellegrino, T. Pessi, M. Pursiainen, A. Rest, E. J. Ridley, B. J. Shappee, X. Sheng, G. P. Smith, G. Terreran, M. A. Tucker, J. Vinkó, R. J. Wainscoat, P. Wiseman, D. R. Young
Figure caption: Top left: fit to the AT 2022aedm host galaxy SED using PROSPECTOR. Top right: host galaxy color image. Bottom row: elliptical host galaxies and offsets of two other luminous fast-cooling transients with unusual spectra (Vinkó et al. 2015; Ho et al. 2023). Images are from Pan-STARRS and centered at the transient positions.
Paper: CUTE Reveals Escaping Metals in the Upper Atmosphere of the Ultrahot Jupiter WASP-189b
Authors: A. G. Sreejith, Kevin France, Luca Fossati, Tommi T. Koskinen, Arika Egan, P. Wilson Cauley, Patricio. E. Cubillos, S. Ambily, Chenliang Huang, Panayotis Lavvas, Brian T. Fleming, Jean-Michel Desert, Nicholas Nell, Pascal Petit, Aline Vidotto
Figure caption: NUV white-light curve fitting of WASP-189b. The top panels show the raw light curve. The bottom panels show the systematics-corrected light curves following the best BIC/best AICc. The solid orange lines denote the transit model of the best fit. The data points are colored based on the CUTE satellite orbits (from purple to yellow in increasing order).
Paper: CUTE Reveals Escaping Metals in the Upper Atmosphere of the Ultrahot Jupiter WASP-189b
Authors: A. G. Sreejith, Kevin France, Luca Fossati, Tommi T. Koskinen, Arika Egan, P. Wilson Cauley, Patricio. E. Cubillos, S. Ambily, Chenliang Huang, Panayotis Lavvas, Brian T. Fleming, Jean-Michel Desert, Nicholas Nell, Pascal Petit, Aline Vidotto
Figure caption: Top: transmission spectrum at 10 Å bin. Bottom: transmission spectrum at 100 Å bin.
Paper: Self-consistent 3D Radiative Transfer for Kilonovae: Directional Spectra from Merger Simulations
Authors: Luke J. Shingles, Christine E. Collins, Vimal Vijayan, Andreas Flörs, Oliver Just, Gerrit Leck, Zewei Xiong, Andreas Bauswein, Gabriel Martínez-Pinedo, Stuart A. Sim
Figure caption: Left panel: synthetic direction-integrated bolometric luminosity (all wavelengths excluding γ-rays), global deposition rate for γ-rays, and emission and deposition rates for β − particles for the 3D AD2 model. Right panel: global thermalization ratios (power deposited divided by emitted) vs. time for γ-rays and β − and α particles in the 3D AD2 ARTIS model. We also show the Barnes et al. (2016) analytical fits (Equations (C1) and (C2)) for comparison.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Same as Figure 2 but comparing the z ∼ 2, 1, and 0 distributions (from left to right). The comoving field of view is kept consistent across images at different redshifts. The gas temperature maps show that, across all models, the inner CGM transitions from an unstable state with supersonic cold gas inflows to a stable virialized state dominated by hot-mode accretion. The timing of this transition is influenced by the gravitational potential of the halo and cooling physics. The transition time is comparable for ADM-1, CDM, and CDM-NF simulations due to their comparable cooling functions. The transition appears to be delayed in ADM-2 due to its significantly higher cooling rate. A minor difference between CDM simulations (both CDM and CDM-NF) and ADM-1 is the multiphase structure of the CGM, which arises from helium and metal cooling peaks in the cooling function that leads to thermal instabilities. CDM displays a chaotic gas distribution near the galactic center at z ∼ 2 due to feedback, which settles down to a disk by z ≤ 1. In contrast, ADM-1, ADM-2, and CDM-NF feature early-settled disks at z ∼ 2, which are then disturbed by galaxy mergers and cold filaments of accreted gas at around z ∼ 1. The final gas distributions in ADM-1 and CDM-NF are more compact. However, ADM-2, which has strong cooling rates and late-time gas accretion, maintains an extended gas disk at z ∼ 0 similar to baryons in CDM. Videos of the simulations are available at https://rb.gy/et2q0.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Same as the z ∼ 0 density distributions in Figure 3 but supplemented with the CDM densities in the top row. Videos of the simulations are available at https://rb.gy/et2q0.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Same as Figure 3 but for z ∼ 1. The top row also provides the density distributions for CDM. Videos of the simulations are available at https://rb.gy/et2q0.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Plot of the central mass contained in the inner 0.5 kpc of each simulated galaxy as a function of redshift. The ADM dominates the inner galactic density at redshifts z ≳ 3 and enhances the central densities of baryons and CDM in both ADM-1 and ADM-2 compared to CDM. Note that there is a sharp dip in the enclosed mass for ADM-2 species at z ≈ 3.3 because a large merger temporarily perturbed the central galaxy and the center-finding algorithm locked onto a smaller-mass galaxy.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Surface density profiles in the galactic stellar disk plane using a cylindrical region with ∣z∣ ≤ 200 pc for ADM species (first two panels) and all DM (CDM for CDM and CDM-NF and CDM+ADM for ADM-1 and ADM-2).
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Density profiles for ADM species (first two panels) and all DM (CDM for CDM and CDM-NF and CDM+ADM for ADM-1 and ADM-2).
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Density profiles for baryons and CDM.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Circular velocities (﹩\sqrt{{GM}(\lt R)/R}﹩) for each simulation.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Half-mass heights z 1/2 for ADM in the galactic stellar disk plane computed using a cylindrical volume with ∣z∣ ≤ 5 kpc.
Paper: AT 2022aedm and a New Class of Luminous, Fast-cooling Transients in Elliptical Galaxies
Authors: M. Nicholl, S. Srivastav, M. D. Fulton, S. Gomez, M. E. Huber, S. R. Oates, P. Ramsden, L. Rhodes, S. J. Smartt, K. W. Smith, A. Aamer, J. P. Anderson, F. E. Bauer, E. Berger, T. de Boer, K. C. Chambers, P. Charalampopoulos, T.-W. Chen, R. P. Fender, M. Fraser, H. Gao, D. A. Green, L. Galbany, B. P. Gompertz, M. Gromadzki, C. P. Gutiérrez, D. A. Howell, C. Inserra, P. G. Jonker, M. Kopsacheili, T. B. Lowe, E. A. Magnier, C. McCully, S. L. McGee, T. Moore, T. E. Müller-Bravo, M. Newsome, E. Padilla Gonzalez, C. Pellegrino, T. Pessi, M. Pursiainen, A. Rest, E. J. Ridley, B. J. Shappee, X. Sheng, G. P. Smith, G. Terreran, M. A. Tucker, J. Vinkó, R. J. Wainscoat, P. Wiseman, D. R. Young
Figure caption: Spectroscopic analysis of AT 2022aedm. Left: line identification in the highest signal-to-noise ratio spectra. No unambiguous broad features are identified, but we clearly detect early emission lines of Hα and He II and, at later times, blueshifted absorption lines of H and He I. Right: comparison of AT 2022aedm with other fast transients. Dougie and AT 2020bot also show a lack of obvious SN features and occurred in similar environments to AT 2022aedm.
Paper: AT 2022aedm and a New Class of Luminous, Fast-cooling Transients in Elliptical Galaxies
Authors: M. Nicholl, S. Srivastav, M. D. Fulton, S. Gomez, M. E. Huber, S. R. Oates, P. Ramsden, L. Rhodes, S. J. Smartt, K. W. Smith, A. Aamer, J. P. Anderson, F. E. Bauer, E. Berger, T. de Boer, K. C. Chambers, P. Charalampopoulos, T.-W. Chen, R. P. Fender, M. Fraser, H. Gao, D. A. Green, L. Galbany, B. P. Gompertz, M. Gromadzki, C. P. Gutiérrez, D. A. Howell, C. Inserra, P. G. Jonker, M. Kopsacheili, T. B. Lowe, E. A. Magnier, C. McCully, S. L. McGee, T. Moore, T. E. Müller-Bravo, M. Newsome, E. Padilla Gonzalez, C. Pellegrino, T. Pessi, M. Pursiainen, A. Rest, E. J. Ridley, B. J. Shappee, X. Sheng, G. P. Smith, G. Terreran, M. A. Tucker, J. Vinkó, R. J. Wainscoat, P. Wiseman, D. R. Young
Figure caption: Follow-up of AT 2022aedm. Left: multicolor light curves from UV to NIR. Arrows indicate upper limits. The inset shows the early ATLAS flux data with a second-order fit (also shown on the multicolor plot) and time above half-maximum. Taking the shallowest and steepest rises allowed by the ATLAS data changes the time of zero flux by ≲0.5 days. Right: spectroscopic follow-up. Spectra are labeled by telescope/instrument and time since explosion in the rest frame. The photometric data shown on the left are available as the data behind the figure.(The data used to create this figure are available.)
Paper: AT 2022aedm and a New Class of Luminous, Fast-cooling Transients in Elliptical Galaxies
Authors: M. Nicholl, S. Srivastav, M. D. Fulton, S. Gomez, M. E. Huber, S. R. Oates, P. Ramsden, L. Rhodes, S. J. Smartt, K. W. Smith, A. Aamer, J. P. Anderson, F. E. Bauer, E. Berger, T. de Boer, K. C. Chambers, P. Charalampopoulos, T.-W. Chen, R. P. Fender, M. Fraser, H. Gao, D. A. Green, L. Galbany, B. P. Gompertz, M. Gromadzki, C. P. Gutiérrez, D. A. Howell, C. Inserra, P. G. Jonker, M. Kopsacheili, T. B. Lowe, E. A. Magnier, C. McCully, S. L. McGee, T. Moore, T. E. Müller-Bravo, M. Newsome, E. Padilla Gonzalez, C. Pellegrino, T. Pessi, M. Pursiainen, A. Rest, E. J. Ridley, B. J. Shappee, X. Sheng, G. P. Smith, G. Terreran, M. A. Tucker, J. Vinkó, R. J. Wainscoat, P. Wiseman, D. R. Young
Figure caption: Photometric comparison of AT 2022aedm and other fast transients. For visual clarity, we plot the uncertainties only for AT 2022aedm. Left: absolute rest-frame light curves. Right: g − r color evolution.
Paper: AT 2022aedm and a New Class of Luminous, Fast-cooling Transients in Elliptical Galaxies
Authors: M. Nicholl, S. Srivastav, M. D. Fulton, S. Gomez, M. E. Huber, S. R. Oates, P. Ramsden, L. Rhodes, S. J. Smartt, K. W. Smith, A. Aamer, J. P. Anderson, F. E. Bauer, E. Berger, T. de Boer, K. C. Chambers, P. Charalampopoulos, T.-W. Chen, R. P. Fender, M. Fraser, H. Gao, D. A. Green, L. Galbany, B. P. Gompertz, M. Gromadzki, C. P. Gutiérrez, D. A. Howell, C. Inserra, P. G. Jonker, M. Kopsacheili, T. B. Lowe, E. A. Magnier, C. McCully, S. L. McGee, T. Moore, T. E. Müller-Bravo, M. Newsome, E. Padilla Gonzalez, C. Pellegrino, T. Pessi, M. Pursiainen, A. Rest, E. J. Ridley, B. J. Shappee, X. Sheng, G. P. Smith, G. Terreran, M. A. Tucker, J. Vinkó, R. J. Wainscoat, P. Wiseman, D. R. Young
Figure caption: Results from fitting the multiband photometry with SUPERBOL. Left: bolometric and pseudobolometric (optical) light curves compared to AT 2018cow, AT 2020bot, and Dougie. We also show a representative SN Ia (Nugent et al. 2011) and an SLSN sample (Nicholl et al. 2015). For visual clarity, we plot the uncertainties only for AT 2022aedm. Right: temperature and radius evolution from blackbody fits, together with the best-fitting power laws. The orange lines are not fit to the first two data points, for which no UV or NIR data are available.
Paper: Three-dimensional Turbulent Reconnection within the Solar Flare Current Sheet
Authors: Yulei Wang, Xin Cheng, Mingde Ding, Zhaoyuan Liu, Jian Liu, Xiaojue Zhu
Figure caption: Temporal evolutions of turbulent magnetic energy and 2D spectra. (a) The distributions of turbulent magnetic energy near the CS center. The three columns show the E  M  distribution at x = −0.005, 0, and 0.005 planes. The gray arrows depict the in-plane magnetic field. (b) The distributions of ﹩{E}_{M}^{F}\left({k}_{z},{k}_{y}\right)﹩ at the CS (left) and the loop-top regions (right). For both (a) and (b), the four rows correspond to four moments of t = 6.10, 6.80, 7.50, and 8.20.
Paper: Three-dimensional Turbulent Reconnection within the Solar Flare Current Sheet
Authors: Yulei Wang, Xin Cheng, Mingde Ding, Zhaoyuan Liu, Jian Liu, Xiaojue Zhu
Figure caption: Numerical convergences of reconnection rate and turbulent spectra. (a) The temporal evolution of the reconnection rate for four cases with different resolutions and Lundquist numbers. The time-averaged reconnection rates are estimated in the time domain ﹩t\in \left[5,8.2\right]﹩. (b) and (c) The spectra of turbulent magnetic energy at t = 8.2 in the CS (b) and at the loop-top region (c) for four different cases.
Paper: Three-dimensional Turbulent Reconnection within the Solar Flare Current Sheet
Authors: Yulei Wang, Xin Cheng, Mingde Ding, Zhaoyuan Liu, Jian Liu, Xiaojue Zhu
Figure caption: Synthesized images of four cases at t  = 8.2. (a) The face-on views of the flare CS as observed by the XRT Al-poly/open channel. (b) The face-on views as observed by the AIA 94 Å channel.
Paper: Disentangling the Hadronic Components in NGC 1068
Authors: Marco Ajello, Kohta Murase, Alex McDaniel
Figure caption: Model spectra of MeV–TeV gamma-ray emission from NGC 1068, compared to Fermi LAT data obtained by this work (black data points). AGN corona (Murase et al. 2020; Murase 2022) and starburst (Ajello et al. 2020; and see also the main text) models are shown by red and blue shaded bands, respectively. The all-flavor coronal neutrino spectrum, which can account for the IceCube data (gray shaded band; IceCube Collaboration et al. 2022), is also shown with the black thin solid curve (Murase et al. 2020). Sensitivity curves of AMEGO-X (Caputo et al. 2022) and e-ASTROGAM (De Angelis et al. 2017) are also overlaid.
Paper: Disentangling the Hadronic Components in NGC 1068
Authors: Marco Ajello, Kohta Murase, Alex McDaniel
Figure caption: A 95% positional uncertainty ellipse for NGC 1068 in the 50 MeV–1 TeV energy range as derived in this analysis overlaid on an image from the VLT.
Paper: Disentangling the Hadronic Components in NGC 1068
Authors: Marco Ajello, Kohta Murase, Alex McDaniel
Figure caption: Yearly lightcurve of NGC 1068 at low (50–500 MeV, blue) and high (500 MeV–1 TeV, orange) energies.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Four panels displaying the temperature and surface density distributions of ADM gas in ADM-1 and ADM-2 (left panels) and baryonic gas in CDM and CDM-NF (right panels). The left side of each panel shows the gas temperature distribution on the CGM scale at z ∼ 1 (350 comoving  kpc field of view). It is overlaid with the velocity field of the gas, where darker streamlines indicate higher velocities. Cooling physics and gravity determine the thermal properties of gas at this scale. Due to an order-of-magnitude stronger cooling efficiency, the ADM gas in ADM-2 is distinct from the other three cases, exhibiting stronger cooling flows at z ∼ 1 and delayed inner CGM virialization. The right side of each panel shows the surface density of cold, neutral gas in the central halo (30 comoving  kpc field of view). Both face-on and edge-on views are shown. The neutral gas distributions are sensitive to gas accretion from the CGM, feedback from star formation (relevant for baryonic gas in the CDM,  ADM-1, and ADM-2  simulations), and the thermal instability of the gas. For baryons in CDM, an extended, corotating gaseous disk already forms at z ∼ 1. For ADM-1 and ADM-2, we find compact ADM gas disks surrounded by streams of cold gas accreted from the CGM with poor alignment to the angular momentum of the central disk. The baryons in CDM-NF exhibit a more extended gas disk than the ADM cases at this redshift, likely due to enhanced accretion via the helium peak in Figure 1. Figure D2 provides the corresponding panels for z ∼ 2 and z ∼ 0. Videos of the simulations are available at https://rb.gy/et2q0.
Paper: Simulating Atomic Dark Matter in Milky Way Analogs
Authors: Sandip Roy, Xuejian Shen, Mariangela Lisanti, David Curtin, Norman Murray, Philip F. Hopkins
Figure caption: Atomic cooling rates for baryons (green line) and the ADM benchmarks, ADM-1 and ADM-2, which are defined in Table 1 (dotted and dashed orange lines, respectively). The upper axis translates the temperature T to the virial temperature of a galaxy with virial mass M vir (Bryan & Norman 1998). Rates are normalized by the particle number density to separate the effect of absolute density and mass on the shapes of the curves. The ADM cooling rates increase with decreasing dark electron mass and increasing dark fine-structure coupling. The cutoff temperature scales like the hydrogen binding energy. Compared to ADM-1, ADM-2 gas accretes more rapidly into the inner galaxy but is also more resistant to fragmentation due to its larger binding energy.