adsabs/AstroCLIMB huggingface dataset:
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: Baryon and ADM density projection plots at the present day. The different simulations are organized by column, while the types of species are organized by rows. Gas is presented face-on, while stars and ADM clumps are presented edge-on. The ADM gas disk in ADM-1 is as compact as the baryonic disk in CDM-NF because both gas species have similar cooling rates and binding energies and lack feedback. The ADM gas disk in ADM-2 undergoes enhanced accretion and is also more resistant to fragmentation, making it less compact. In both ADM-1 and ADM-2, ∼95% of the inner ADM is in the form of clumps, which are concentrated in the most central regions of the galaxy. Because of the lack of feedback, the ADM clumps in ADM-1 and ADM-2 and the baryonic stars in CDM-NF lack a prominent thin disk and are more centrally concentrated. The large central densities of ADM in ADM-1 and ADM-2 enhance the central baryonic densities as well, and in the case of ADM-2, the baryonic gas disk collapses catastrophically. Figures D3 and D4 provide the density distributions for additional redshifts, as well as 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: Left panel: comparison between the cooling rates used in GIZMO (Hopkins et al. 2018b), excluding metals like helium, and those of Rosenberg & Fan (2017) with ﹩{m}_{e^{\prime} }={m}_{{\rm{e}}}﹩, ﹩{m}_{p^{\prime} }={m}_{{\rm{p}}}﹩, and ﹩\alpha ^{\prime} =\alpha ﹩. As in Figure 1, the upper axis translates the ADM temperature T to the virial temperature of a galaxy with virial mass M vir (Bryan & Norman 1998). These curves agree to ﹩{ \mathcal O }(1)﹩, which is sufficient for the purposes of this investigation. Right panel: breakdown of the contribution of different cooling processes to the total Rosenberg & Fan (2017) cooling rate in the left panel. Collisional excitation dominates at low ADM temperatures, ﹩{\mathrm{log}}_{10}(T/\,{\rm{K}})\in \{4.2,5.0\}﹩, while bremsstrahlung (i.e., free–free cooling) dominates at high temperatures, T ≳ 106 K.
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: Top panel: formation history for baryonic stars and ADM clumps in the inner 10 kpc for all simulations. Colors represent the particle species, and line styles represent the simulation. Above the figure are red–green–blue synthetic images for particles of different ages (see the legend). The baryonic stars in CDM-NF and the ADM clumps in ADM-1 and ADM-2 have greater formation probabilities at z ≳ 2 compared to baryonic stars in CDM. This is also evident in the corresponding color maps, which are red-dominant compared to those of the stars in CDM. Bottom panel: enclosed mass profiles for all species at z ∼ 0. The solid, dotted, and dashed lines reference the CDM, ADM-1, and ADM-2 simulations, respectively. The different colors represent the separate particle species. The ADM is concentrated within the inner ∼kiloparsec of the galaxy, with an enclosed mass comparable to that of baryons. The presence of this additional mass causes an overall enhancement in the baryonic and CDM mass in the central 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: Left panel: cooling rates with varying ﹩{m}_{e^{\prime} }﹩ and fixed ﹩\alpha ^{\prime} =\alpha ﹩. As in Figures 1 and A1, the upper axis translates the ADM temperature T to the virial temperature of a galaxy with virial mass M vir (Bryan & Norman 1998). As ﹩{m}_{e^{\prime} }﹩ is reduced, the cutoff temperature decreases, since it scales as the dark hydrogen binding energy, which is proportional to ﹩{m}_{e^{\prime} }﹩. The peak cooling rates increase because less massive electrons interact more efficiently. Right panel: cooling rates with varying ﹩\alpha ^{\prime} ﹩ and fixed ﹩{m}_{e^{\prime} }={m}_{e}﹩. As ﹩\alpha ^{\prime} ﹩ decreases, the ADM cutoff temperature decreases because the dark hydrogen binding energy scales as ﹩\alpha {{\prime} }^{2}﹩. The peak cooling rates also decrease for weaker coupling constants.
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: Orbital circularity probability density functions for baryonic stars and ADM clumps in CDM, CDM-NF, ADM-1, and ADM-2 at z ∼ 0. Orbital circularities in the ranges ϵ ≥ 0.8, 0.2 < ϵ < 0.8, and ϵ < 0.2 resemble a thin disk, thick disk, and spheroid, respectively. Baryonic stars in the CDM, ADM-1, and ADM-2 simulations have dominant thin disks, while those in CDM-NF have more prominent thick disks. The same holds for feedback-less ADM clumps in ADM-1 and ADM-2.
Paper: Snowflakes in a Furnace: Formation of CO and Dust in a Recurrent Nova Eruption
Authors: D. P. K. Banerjee, C. E. Woodward, V. Joshi, A. Evans, F. M. Walter, G. H. Marion, E. Y. Hsiao, N. M. Ashok, R. D. Gehrz, S. Starrfield
Figure caption: Schematic of the V745 Sco system with the equatorial density enhancement (EDE) that collimates the ejecta into a bipolar flow. The forward and reverse shocks (FS, RS) are shown with a cold clumpy shell in between that is proposed to be the site of the CO and dust formation. The positions and sizes of the WD, RG, and shock region are roughly to the following scale (Section 2.3), viz. R RG = 290 R ⊙, R WD = 65 R ⊙ (at outburst; Orlando et al. 2017), WD to RG separation = 810  R ⊙, and inner Lagrangian point (L1) ∼450  R ⊙ from the WD. The distance of the FS from the WD is shown at 1070  R ⊙ assuming a representative value of the shock velocity, v  s  = 1000 km s−1. The actual distance lies at 2000  R ⊙, almost twice that shown. The shape of the EDE, as shown here, is only schematic.
Paper: Snowflakes in a Furnace: Formation of CO and Dust in a Recurrent Nova Eruption
Authors: D. P. K. Banerjee, C. E. Woodward, V. Joshi, A. Evans, F. M. Walter, G. H. Marion, E. Y. Hsiao, N. M. Ashok, R. D. Gehrz, S. Starrfield
Figure caption: High-resolution spectra (R = 120,000) of V745 Sco obtained on the Cerro Tololo 1.3 m (+CHIRON) on 2014 February 16 (∼+10 days past outburst) showing coronal lines from highly ionized species. The Hα profile in the bottom right panel is from 2014 February 9 (∼3 days after the outburst) and shows structures that are discussed in the text.
Paper: Snowflakes in a Furnace: Formation of CO and Dust in a Recurrent Nova Eruption
Authors: D. P. K. Banerjee, C. E. Woodward, V. Joshi, A. Evans, F. M. Walter, G. H. Marion, E. Y. Hsiao, N. M. Ashok, R. D. Gehrz, S. Starrfield
Figure caption: The top left and right panels show the JHK(L) light curves from the 1989 (Sekiguchi et al. 1990) and the 2014 (ANDICAM data) eruptions, respectively. The error bars in the plots are smaller than the symbol sizes. An IR excess due to dust is seen around day 9. The bottom panel shows the SED of the excess fitted with model fits of silicate (red) and amorphous carbon (blue) dust.
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 left panel: the integrated intensity map of the 110,11–101,10A line (color) over the 1.2 mm continuum (contour). The contour levels for the continuum emission are 2.5, 4.9, 9.5, 18.6, 36.3, and 70.8 mJy beam−1. Rest of the panels: the channel map of 110,11–101,10A in units of T b (color) and the 83,5–82,6A line (contour). The contour levels for the 83,5–82,6A emission are 15, 40, 65, and 85 K. The beam sizes are presented in the lower left corner of each channel (Table 1). Inset figures in 4.5 and 5.1 km s−1 channels depict the zoomed-in view of the magenta box (110,11–101,10A line in both color and contour) to present the high-resolution data obtained from both compact and extended configuration combined observation. The contour levels for the 110,11–101,10A emission in the inset figures are 150, 300, 530, and 830 K.
Paper: Dispersive Suprathermal Ion Events Observed by the Parker Solar Probe Mission
Authors: S. T. Alnussirat, R. Livi, D. E. Larson, A. Rahmati, P. L. Whittlesey, O. Romeo, S. T. Badman, Milo Buitrago-Casas, Juan Carlos Martínez Oliveros, M. Pulupa, S. D. Bale, J. Huang, J. Verniero, N. Raouafi, Donald Mitchell, D. J. McComas, Matt Hill, Christina Cohen
Figure caption: Summary of potential sources and PSP magnetic connectivity. An AIA 94 Å image of the Sun on 2022 February 27 at 08:59:59 UTC shows five potential active regions labeled 1–5. A potential field source surface model is used to estimate coronal holes (red and blue patches) and the topology of the neutral line. The instantaneous magnetic field line connecting to PSP is shown in red and attached to a small positive polarity equatorial coronal hole near the west limb.
Paper: Dispersive Suprathermal Ion Events Observed by the Parker Solar Probe Mission
Authors: S. T. Alnussirat, R. Livi, D. E. Larson, A. Rahmati, P. L. Whittlesey, O. Romeo, S. T. Badman, Milo Buitrago-Casas, Juan Carlos Martínez Oliveros, M. Pulupa, S. D. Bale, J. Huang, J. Verniero, N. Raouafi, Donald Mitchell, D. J. McComas, Matt Hill, Christina Cohen
Figure caption: A summary of the 2022 February 27 LED-Ions event. The first panel shows the PSP distance to the Sun in units of solar radii. Panel (2) shows the high-frequency FIELDS radio observations. Panel (3) shows the time series of EPI-Lo and SPAN-I measured differential energy-flux, and panel (4) shows the PSP Carrington longitude.
Paper: Dispersive Suprathermal Ion Events Observed by the Parker Solar Probe Mission
Authors: S. T. Alnussirat, R. Livi, D. E. Larson, A. Rahmati, P. L. Whittlesey, O. Romeo, S. T. Badman, Milo Buitrago-Casas, Juan Carlos Martínez Oliveros, M. Pulupa, S. D. Bale, J. Huang, J. Verniero, N. Raouafi, Donald Mitchell, D. J. McComas, Matt Hill, Christina Cohen
Figure caption: The energy spectra as a function of time for the 2022 February 27 event as seen in SPAN-I.
Paper: Dispersive Suprathermal Ion Events Observed by the Parker Solar Probe Mission
Authors: S. T. Alnussirat, R. Livi, D. E. Larson, A. Rahmati, P. L. Whittlesey, O. Romeo, S. T. Badman, Milo Buitrago-Casas, Juan Carlos Martínez Oliveros, M. Pulupa, S. D. Bale, J. Huang, J. Verniero, N. Raouafi, Donald Mitchell, D. J. McComas, Matt Hill, Christina Cohen
Figure caption: The energy dispersion curve of the proton beam (blue) and the bulk of solar wind (orange).
Paper: Dispersive Suprathermal Ion Events Observed by the Parker Solar Probe Mission
Authors: S. T. Alnussirat, R. Livi, D. E. Larson, A. Rahmati, P. L. Whittlesey, O. Romeo, S. T. Badman, Milo Buitrago-Casas, Juan Carlos Martínez Oliveros, M. Pulupa, S. D. Bale, J. Huang, J. Verniero, N. Raouafi, Donald Mitchell, D. J. McComas, Matt Hill, Christina Cohen
Figure caption: Small-scale coronal jets.
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: Observational characteristics of flare turbulent reconnection. (a) Synthesized XRT Al-poly/open images of the edge-on (left panel) and face-on (right panel) CS and flare loops at t = 8.2. In the left panel, the gray curves depict the z-averaged in-plane magnetic field, the yellow star represents the principal reconnection point of the mean magnetic field, and the cyan and purple dashed lines schematically plot the positions of slow shocks and the loop-top termination shock predicted by the standard flare model, respectively. The principal reconnection point is identified as the position with the maximum z-averaged out-of-plane current density ﹩{\bar{J}}_{z}﹩ (Wang et al. 2021). The magenta and green dashed lines in the face-on image mark the positions of bright structure (BS) and dark structure (DS) in Figure 5, respectively. The units of length is L 0 = 5 × 109 cm. (b) The edge-on view of the reconnecting CS and flare loops at 17:15:29 UT on 2017 September 10 observed by the XRT. (c) The face-on view of the flare at 05:22:50 UT on 2012 January 1 observed by the XRT.
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 evolution of turbulent reconnection at the CS and loop top. (a) The temporal evolution of volume-averaged effective magnetic energy release rates at the CS (blue solid curve) and loop top (blue dashed curve). The orange curve displays the evolution of the reconnection rate. (b) and (c) The power spectra of turbulent magnetic energy at the CS and loop top at selected moments as denoted by different colors. The oblique dashed line denotes the classic spectral index of −5/3 as predicted in theory.
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: Evidence for horizontal flux ropes taking place with kink instability at t = 5.7. (a) The same content as Figure 2(a) but at a different moment (t = 5.7). The colored lines denote three slits across the axes of two flux ropes. (b) The profiles of T, B  x , B  y , B  z , and ﹩{B}_{{xy}}=\sqrt{{B}_{x}^{2}+{B}_{y}^{2}}﹩ along the vertical slit. The purple and green shades highlight the regions of flux ropes 1 and 2, respectively. (c )and (d) The profiles of T, B  x , B  y , B  z , and B  xy  along the purple and green horizontal slits.
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 fraction of ADM mass (gas and clumps) to CDM mass at heights of ∣z∣ ≤ 0.2 and 1 kpc in the galactic stellar disk plane. At the solar radius (≈8 kpc), we find that the surface density fractions are below unity and the constrained fractions in Schutz et al. (2018), Buch et al. (2019), and Read (2014).
Paper: Flyby Galaxy Encounters with Multiple Black Holes Produce Star-forming Linear Features
Authors: Nianyi Chen, Patrick LaChance, Yueying Ni, Tiziana Di Matteo, Rupert Croft, Priyamvada Natarajan, Simeon Bird
Figure caption: Target galaxies for the search for runaway BHs and SFLFs (orange points), plotted on top of the distribution of all galaxies with M gal > 5 × 108 M ⊙ in ASTRID at z = 2. The two systems with the most prominent SFLFs are shown as stars (z ∼ 2 system in blue, z ∼ 1 system in red). We focus our search among the star-forming (SFR > 1 M ⊙ yr−1), compact (r half < 2 kpc) galaxies with masses 5 × 109 M ⊙ < M gal < 5 × 1010 M ⊙ that contain at least three BHs with a central M BH > 107 M ⊙ BH, as indicated by the gray dashed lines.
Paper: Flyby Galaxy Encounters with Multiple Black Holes Produce Star-forming Linear Features
Authors: Nianyi Chen, Patrick LaChance, Yueying Ni, Tiziana Di Matteo, Rupert Croft, Priyamvada Natarajan, Simeon Bird
Figure caption: First and second rows: stars (first row; color-coded by age) and gas (second row; color-coded by temperature) associated with the SFLFs at z ∼ 2 (left) and 1 (right). The features extend to ∼50 kpc from the compact galaxy on the left of each image. Third row: mock image of the systems in the HST F606W and F814W filters. Fourth row: F606W–F814W color of the stellar population, modeled with the Python-FSPS stellar population model (Conroy & Gunn 2010), and the mean age of the 5% youngest stars. In the fifth row, the mock image of the systems in the JWST filters will reveal the older stellar population along the SFLFs.
Paper: Flyby Galaxy Encounters with Multiple Black Holes Produce Star-forming Linear Features
Authors: Nianyi Chen, Patrick LaChance, Yueying Ni, Tiziana Di Matteo, Rupert Croft, Priyamvada Natarajan, Simeon Bird
Figure caption: Example runaway BH involved in an MBH triplet (marked by red, green, and blue crosses) identified in ASTRID at z ∼ 1.7. The red cross is the BH that got ejected from the host galaxy with a velocity of ∼700 km s−1 due to the complex dynamics within the halo. The host galaxy mass is M gal = 1.3 × 1011 M ⊙, the runaway BH has a mass of M BH = 1.3 × 107 M ⊙, and the central BH (blue cross) has M BH = 6.6 × 108 M ⊙.
Paper: Flyby Galaxy Encounters with Multiple Black Holes Produce Star-forming Linear Features
Authors: Nianyi Chen, Patrick LaChance, Yueying Ni, Tiziana Di Matteo, Rupert Croft, Priyamvada Natarajan, Simeon Bird
Figure caption: Time evolution of the two galaxies involved in producing the SFLF (projected face-on) and the associated BHs (central BH in galaxy 1 in blue, two BHs in the tidally disrupted galaxy in green and magenta, and another BH nearby in red). The green line traces the trajectory of BH2 relative to BH1, and the red line shows the orbit of BH3 relative to BH2.
Paper: Flyby Galaxy Encounters with Multiple Black Holes Produce Star-forming Linear Features
Authors: Nianyi Chen, Patrick LaChance, Yueying Ni, Tiziana Di Matteo, Rupert Croft, Priyamvada Natarajan, Simeon Bird
Figure caption: Properties of the three BHs along the SFLFs. The top two panels show the X-ray luminosities and BH masses of the three BHs. The bottom panel shows the distance between the three BHs.
Paper: The Time Evolution of ﹩{M}_{d}/\dot{M}﹩ in Protoplanetary Disks as a Way to Disentangle between Viscosity and MHD Winds
Authors: Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Benoît Tabone, Carlo F. Manara, Marco Tazzari
Figure caption: Time evolution of the mean (top) and width (bottom) of the distribution of t lt for a synthetic population of protoplanetary disks. The solid lines represent the median values, while the shades cover the interval between the 25th and 75th percentiles out of 100 simulations (to account for the statistical effect of disk removal). The blue and yellow lines refer to the viscous and MHD model, respectively, with the lighter shades including the observational uncertainty. While the mean value of the distributions is not much affected by the presence of such uncertainty or the choice of the model, the spread shows quite some difference, exhibiting significantly higher values in the MHD than in the viscous case. The dashed line in the bottom panel marks the observational uncertainty.
Paper: The Time Evolution of ﹩{M}_{d}/\dot{M}﹩ in Protoplanetary Disks as a Way to Disentangle between Viscosity and MHD Winds
Authors: Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Benoît Tabone, Carlo F. Manara, Marco Tazzari
Figure caption: Time evolution of the skewness of the distribution of t lt for a synthetic population of protoplanetary disks, with the same color coding as Figure 2. Both panels show the comparison between the viscous and MHD models, without (left) and with (right) the additional observational uncertainty σ obs. Despite the theoretical predictions of the two models being significantly different (left panel), the convolution with observational biases completely smooths them out (right panel).
Paper: The Time Evolution of ﹩{M}_{d}/\dot{M}﹩ in Protoplanetary Disks as a Way to Disentangle between Viscosity and MHD Winds
Authors: Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Benoît Tabone, Carlo F. Manara, Marco Tazzari
Figure caption: Time evolution of a synthetic population of disks, evolved via viscosity (top) or MHD winds (bottom), in the ﹩{M}_{d}{\textstyle \mbox{--}}\dot{M}﹩ plane. The solid lines show the theoretical isochrones at ages 0.1, 1, and 10 Myr as per the legend, while the disks in the population at each age are represented by dots with the same color coding. While viscous disks tend to converge to the same isochrone at evolved stages, MHD disks show a larger dispersion.
Paper: The Time Evolution of ﹩{M}_{d}/\dot{M}﹩ in Protoplanetary Disks as a Way to Disentangle between Viscosity and MHD Winds
Authors: Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Benoît Tabone, Carlo F. Manara, Marco Tazzari
Figure caption: Disk and accretion fraction (left and right panel, respectively) in our viscous (light blue), MHD (orange), and viscous+photoevaporation (lilac) simulations, compared with data by Hernández et al. (2007) and Fedele et al. (2010) (blue squares). The shaded areas are as in Figure 2. The dashed blue lines show the exponential fits to the data. Following the original paper, we define the accretion fraction as the fraction of sources with accretion rate higher than 10−11 M ⊙ yr−1. Our choice of a log-normal distribution of initial accretion timescales for the MHD model reproduces both the disk and accretion fraction, as does the exponential distribution chosen by Tabone et al. (2022b). The viscous model does not reproduce any of the fractions due to the lack of a disk dispersal mechanism, while including internal photoevaporation allows us to recover the observed behavior.
Paper: The Time Evolution of ﹩{M}_{d}/\dot{M}﹩ in Protoplanetary Disks as a Way to Disentangle between Viscosity and MHD Winds
Authors: Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Benoît Tabone, Carlo F. Manara, Marco Tazzari
Figure caption: Comparison of the evolution of the mean (top) and width (bottom) for the viscous (blue) and MHD (yellow) models, including observational uncertainties, with the observations (gray diamonds). The shaded areas are as in Figure 2, while the gray bars represent the interval between the 16th and 84th percentiles (top) and the uncertainty on the width (bottom). While both models overestimate the mean values (see text for details), the evolution of the width of the distribution suggests a better match with the MHD model.
Paper: The Time Evolution of ﹩{M}_{d}/\dot{M}﹩ in Protoplanetary Disks as a Way to Disentangle between Viscosity and MHD Winds
Authors: Alice Somigliana, Leonardo Testi, Giovanni Rosotti, Claudia Toci, Giuseppe Lodato, Benoît Tabone, Carlo F. Manara, Marco Tazzari
Figure caption: Time evolution of a synthetic population of viscous disks in the ﹩{M}_{d}{\textstyle \mbox{--}}\dot{M}﹩ plane (left panel) and corresponding histograms of t lt (right panel). The color coding is as in Figure 1. Full dots represent disks whose initial viscous timescale is shorter than the age of the population and that can therefore be considered evolved.