adsabs/AstroCLIMB huggingface dataset:
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Example of 10 LAEs spectroscopically identified at z ∼ 3.7. The left panel shows the stamp images in five broad bands and the narrowband NB570. The image size is 6″ × 6″. The right panel shows the optical spectra of the LAEs taken by MMT Hectospec. The red vertical lines indicate the positions of the redshifted Lyα lines. A full version of the figure is shown in the Appendix.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Response curves of the narrowband filters (black solid lines) and broadband filters (dashed lines) used in this work. Instrument response has been included for the broad bands. The maximum responses of the narrowband filters are set to 0.8 for the purpose of clarity. The filter NB570 is used to select z ∼ 3.7 LAEs, and the NB704 and NB711 filters are used to select z ∼ 4.8 LAEs.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Same as Figure 3, but for our z ∼ 4.8 LAEs selected in NB704. A full version of the figure is shown in the Appendix.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Redshift distribution of the spectroscopically confirmed LAEs at z ∼ 3.7 (upper panel) and z ∼ 4.8 (lower panel). The dashed lines show the response curves of the narrowband filters.
Paper: A Comprehensive Observational Study of the FRB 121102 Persistent Radio Source
Authors: Ge Chen, Vikram Ravi, Gregg W. Hallinan
Figure caption: Implication from the lack of refractive scintillation modulation assuming a range of distances between the scattering screen and the observer. Upper panel: source radius lower limits in the Ku (dashed–dotted blue line) and K (solid black line) bands, the scattering disk radius at the transitional frequency ν 0, as well as the source radius upper limit from the unresolved VLBI image at 5 GHz. Lower panel: brightness temperature upper limits using the emission region size lower limit inferred from the Ku band (θ  r  ≳ 10 μas) and the weighted average flux densities measured in the Ku (dashed blue line) and K (solid black line) bands.
Paper: A Comprehensive Observational Study of the FRB 121102 Persistent Radio Source
Authors: Ge Chen, Vikram Ravi, Gregg W. Hallinan
Figure caption: Normalized (and scaled) flux density light curve of the K (left) and Ku (right) bands. f3, f2, and f1 represent the flux density of QRS 121102, phase calibrator 2, and phase calibrator 1, respectively. Red open circles (f3) show the normalized flux density of QRS 121102, black open diamonds (f3/f2) show the flux density of QRS 121102 divided by those of phase calibrator 2 and then normalized to average at unity, and blue open squares (f3/f1) are the flux density of QRS 121102 divided by those of phase calibrator 1 and then normalized to average at unity.
Paper: A Comprehensive Observational Study of the FRB 121102 Persistent Radio Source
Authors: Ge Chen, Vikram Ravi, Gregg W. Hallinan
Figure caption: Flux density light curve of the K (left) and Ku (right) bands. f3, f2, f1, and f0 represent the flux density of QRS 121102 (red circles), phase calibrator 2 (black diamonds), phase calibrator 1 (blue squares), and the prime calibrator (cyan stars), respectively. f3 and f2 are scaled by 104 and 10 times for display. Details of the observations are shown in Tables 1 and 2.
Paper: A Comprehensive Observational Study of the FRB 121102 Persistent Radio Source
Authors: Ge Chen, Vikram Ravi, Gregg W. Hallinan
Figure caption: VLA images (in J2000 coordinates) of QRS 121102 in seven epochs, with the band indicated in parentheses. The color scale represents the flux density in janskys per beam (see color bar). The light gray circle (bottom left corner of each image) shows the synthesized beam size (1σ), and the red circle shows the 1σ 2D Gaussian fitting results convolved with the synthesized beam. The position angles of the best-fit results are consistent with those of the clean beams within 1σ in all cases where the source is unresolvable.
Paper: A Comprehensive Observational Study of the FRB 121102 Persistent Radio Source
Authors: Ge Chen, Vikram Ravi, Gregg W. Hallinan
Figure caption: 2D medium-resolution LRIS spectrum of the host galaxy of QRS 121102. Wavelength has been converted to the rest frame using the previously reported redshift of z = 0.19273 (Tendulkar et al. 2017). Top to bottom, the panels are the observed 2D spectrum, the 2D fitting model, and the residual (data−model). On the top and right of each panel are plots of the data collapsed along the wavelength and position axes, respectively.
Paper: A Comprehensive Observational Study of the FRB 121102 Persistent Radio Source
Authors: Ge Chen, Vikram Ravi, Gregg W. Hallinan
Figure caption: Locations of the host, slits, and sources in the low-resolution Keck/LRIS observation. The slit orientations are shown as black lines. Spectra were extracted for each of sources S1, S2, and S3, together with the QRS 121102 host. The background image is an LRIS R-band exposure, as presented in Tendulkar et al. (2017).
Paper: The Maximum Energy of Shock-accelerated Cosmic Rays
Authors: Rebecca Diesing
Figure caption:                    ﹩{E}_{\max }﹩ as a function of shock velocity, (v sh), for a variety of SNRs expanding into media of different ambient density normalizations (color scales), assuming diffusing particles drive magnetic field amplification (left-hand column) or escaping particles drive magnetic field amplification (right-hand column). The top row corresponds to expansion into uniform ambient media and, to be broadly consistent with an SNR from a Type Ia SN, only considers our benchmark scenario. Meanwhile, to capture the wider range of parameters associated with core-collapse SNe, the bottom row corresponds to expansion of SNRs into wind profiles with ﹩{E}_{\mathrm{SN}}\in [1,10]\times {10}^{51}﹩ erg and M ej ∈ [1, 5] M ⊙. Outlined points denote SNRs that are still ejecta-dominated. For SNRs expanding into wind profiles, the evolutionary stage has little bearing on ﹩{E}_{\max }﹩, such that v sh serves as a good predictor of its value (modulo density normalization). Meanwhile, for SNRs expanding into uniform media, v sh is only a good predictor of ﹩{E}_{\max }﹩ during the Sedov–Taylor phase.
Paper: The Maximum Energy of Shock-accelerated Cosmic Rays
Authors: Rebecca Diesing
Figure caption: Cumulative spectra of accelerated protons produced by our benchmark SNR (﹩{E}_{\mathrm{SN}}={10}^{51}﹩ erg, M ej = 1M ⊙) at different stages (denoted by line color) of shock evolution, assuming diffusing particles drive magnetic field amplification (left-hand column) or escaping particles drive magnetic field amplification (right-hand column). The top row of spectra correspond to a uniform ambient medium of density 1 cm−3, while the bottom row correspond to a wind profile of density 3.5(R/pc)−2 cm−3. The maximum proton energy of each spectrum is denoted with a dashed vertical line. Typical SNRs can only accelerate PeV particles if escaping CRs drive magnetic field amplification, and even then only at relatively early times (t ∼ 100 yr).
Paper: The Maximum Energy of Shock-accelerated Cosmic Rays
Authors: Rebecca Diesing
Figure caption: The maximum energy, ﹩{E}_{\max }﹩, accelerated by our benchmark SNR as a function of time, expanding into a uniform medium (red band) and wind profile (blue band), as in Figure 1. The widths of the bands correspond to uncertainties in the nature of CR-driven magnetic field amplification, i.e., the lower (upper) limit assumes diffusing (escaping) particles drive amplification. Blue dotted lines indicate how our wind prediction would change if that wind had a finite size of 1.4 pc, corresponding to a shock age of ∼200 yr. Solid lines give the single-zone ﹩{E}_{\max }﹩ prediction put forth in Bell et al. (2013). While this prediction yields good agreement with our results at early times, we predict a higher ﹩{E}_{\max }﹩ at late times due to the presence of old populations of particles accelerated when the SNR was expanding more rapidly.
Paper: New Insights in the Bubble Wall of NGC 3324: Intertwined Substructures and a Bipolar Morphology Uncovered by JWST
Authors: L. K. Dewangan, A. K. Maity, Y. D. Mayya, N. K. Bhadari, Suman Bhattacharyya, Saurabh Sharma, Gourav Banerjee
Figure caption: (a) Large-scale view of NGC 3324 using a three-color composite map (SUMSS 843 MHz (in red), Herschel 160 μm (in green), and Herschel 70 μm (in blue) images). Squares show the locations of massive O-type stars. Boxes indicate areas that are examined in this work. A solid box encompasses an area presented in Figures A1(b), (c), and (d). (b) A three-color composite map (Herschel 70 μm (in red), Spitzer 8.0 μm (in green), and Spitzer 3.6 μm (in blue) images in linear scale). The area of the image is ∼8.′5 × 9.′8 (central coordinates: α 2000 = 10h36m43.ˢ25; δ 2000 = −58 ° 37′12.″82). All the symbols are the same as presented in Figure 1(a). The dust continuum clumps highlighted by stars are also labeled. (c) Overlay of the SUMSS 843 MHz radio continuum contours on the CHaMP 13CO moment-0 map at [−24.3, −19.9] km s−1. The SUMSS 843 MHz radio continuum contours (see dotted–dashed contours) are plotted with the levels of 46.5, 62.3, 78, 94, 109, and 125 mJy beam−1. The SUMSS contours (see solid contours) are presented with the levels of 132, 141, 157, 172, 188, 204, and 212 mJy beam−1. (d) Herschel dust temperature map. In panels (c) and (d), a thick curve shows the footprint of the sharp edge as seen in Figure A1(b). In panels (b), (c), and (d), a small region (i.e., “sm1”) is indicated by a small yellow box. Scale bars are shown (at 1000″ (or 10.7 pc at a distance of 2.2 kpc) and 120″ (or 1.28 pc)).
Paper: New Insights in the Bubble Wall of NGC 3324: Intertwined Substructures and a Bipolar Morphology Uncovered by JWST
Authors: L. K. Dewangan, A. K. Maity, Y. D. Mayya, N. K. Bhadari, Suman Bhattacharyya, Saurabh Sharma, Gourav Banerjee
Figure caption: (a) The Spitzer-GLIMPSE 5.8 μm image of the bubble rim or NGC 3324 (see the dotted–dashed box in Figure A1(a)). The area of the image is ∼2.′79 × 6.′74 (central coordinates: α 2000 = 10h36m49.ˢ02; δ 2000 = −58 ° 37′25.″52). The positions of four clumps traced in the LABOCA 870 μm continuum map (Duronea et al. 2015) are marked by filled stars. Open circles and open diamonds show the locations of YSOs (from Kuhn et al. 2021) and molecular outflows (from Reiter et al. 2022), respectively. A dotted curve (in red) shows the footprint of the sharp edge. (b) Spitzer-GLIMPSE ratio map of 4.5 μm/3.6 μm emission. (c) The JWST F335M image. In each panel, a small region “sm1” is highlighted by a solid box, and a scale bar shows a size of 0.55 pc at a distance of 2.2 kpc.
Paper: New Insights in the Bubble Wall of NGC 3324: Intertwined Substructures and a Bipolar Morphology Uncovered by JWST
Authors: L. K. Dewangan, A. K. Maity, Y. D. Mayya, N. K. Bhadari, Suman Bhattacharyya, Saurabh Sharma, Gourav Banerjee
Figure caption: (a) A three-color composite map produced using the JWST F470N (in red), F444W (in green), and F335W (in blue) images (see the dotted box in Figure A1(a)). Arrows highlight elongated substructures. (b) A three-color composite map made using the F1800W (in red), F1130W (in green), and F770W (in blue) images. Circles and diamonds show the locations of YSOs and molecular outflows, respectively (see Figure 1(a)). An inset on the lower left presents the region in zoomed-in view (see the solid box in Figure 2(b)). The inset is a two-color composite map produced using the “Edge-DoG”-processed JWST F1800 image (in red) and the JWST F1800 image (in turquoise). In each panel, a scale bar shows a size of 60″ (or 0.64 pc at a distance of 2.2 kpc).
Paper: New Insights in the Bubble Wall of NGC 3324: Intertwined Substructures and a Bipolar Morphology Uncovered by JWST
Authors: L. K. Dewangan, A. K. Maity, Y. D. Mayya, N. K. Bhadari, Suman Bhattacharyya, Saurabh Sharma, Gourav Banerjee
Figure caption: Multiwavelength view of an area “sm1” as indicated by the solid box in Figure 1(a). (a–e) JWST images at F187N, F200W, F335M, F770W, and F1130W are displayed, respectively. (f) A three-color composite map (F1130W (in red), F770W (in green), and F335W (in blue) images in linear scale). (g) F470N−F444W (in linear scale). (h) F444W/F335M (in linear scale). (i) A two-color composite map (F444W/F335M (red) and F470N−F444W (turquoise) images in linear scale). In panels (c), (d), and (g), an arrow shows the position of an OB star candidate (UCAC4 157-048728 or VPHAS-OB1 #03518; Mohr-Smith et al. 2017). In panel (g), three H2 depression regions (i.e., CC-1, CC-2, and CC-3) and one emission structure (FF-1) are labeled. In panel (i), a bipolar morphology is highlighted, and the position of the OB star candidate UCAC4 157-048728 is found at its waist. In each panel, a scale bar corresponding to 20″ (or 0.21 pc at a distance of 2.2 kpc) is drawn.
Paper: New Insights in the Bubble Wall of NGC 3324: Intertwined Substructures and a Bipolar Morphology Uncovered by JWST
Authors: L. K. Dewangan, A. K. Maity, Y. D. Mayya, N. K. Bhadari, Suman Bhattacharyya, Saurabh Sharma, Gourav Banerjee
Figure caption: (a) HST F658N image. A dashed curve (in red) indicates the diffuse emission. (b) JWST F444W image. (c) F470N−F444W (in linear scale). An inset on the upper left shows the region in zoomed-in view (see the solid box in Figure 3(c)). The inset is the “Edge-DoG”-processed F470N−F444W image. In each panel, the scale bar corresponding to 60″ (or 0.64 pc at a distance of 2.2 kpc) is shown.
Paper: New Insights in the Bubble Wall of NGC 3324: Intertwined Substructures and a Bipolar Morphology Uncovered by JWST
Authors: L. K. Dewangan, A. K. Maity, Y. D. Mayya, N. K. Bhadari, Suman Bhattacharyya, Saurabh Sharma, Gourav Banerjee
Figure caption: (a) Same as the inset shown in Figure 2(b). (b) Same as the inset shown in Figure 3(c). (c) The “Edge-DoG”-processed F444W/F335M image (see the solid box in Figure 2(b)). (d) A three-color composite map (“Edge-DoG”-processed F470N−F444W image (in red), the “Edge-DoG”-processed F444W/F335M image (in green), and the HST F658N image (in blue).
Paper: ALMA Observations of Supernova Remnant N49 in the Large Magellanic Cloud. II. Non-LTE Analysis of Shock-heated Molecular Clouds
Authors: H. Sano, Y. Yamane, J. Th. van Loon, K. Furuya, Y. Fukui, R. Z. E. Alsaberi, A. Bamba, R. Enokiya, M. D. Filipović, R. Indebetouw, T. Inoue, A. Kawamura, M. Lakićević, C. J. Law, N. Mizuno, T. Murase, T. Onishi, S. Park, P. P. Plucinsky, J. Rho, A. M. S. Richards, G. Rowell, M. Sasaki, J. Seok, P. Sharda, L. Staveley-Smith, H. Suzuki, T. Temim, K. Tokuda, K. Tsuge, K. Tachihara
Figure caption: Time evolution of kinematic temperature T kin at the cloud center after the supernova event that generates SNR N49. Colors indicate the assumed cosmic-ray ionization rate ζ from 3 × 10−17 s−1 to 1 × 10−14 s−1. The star symbol indicates the observed values of T kin for the ambient or pre-shocked clouds at the age of N49 (4800 yr).
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Development and decay of the CS during flux emergence. The plot from left to right shows the logarithm of the out-of-plane current (top panels) and the radial velocity (bottom panels) at three different times. The first phase is a lengthening and thinning CS. The middle panel shows a well-developed CS undergoing reconnection through tearing. Finally, after the emergence, the CS starts decaying and reconnection stops. Velocity jets can be seen inward to the bipole footpoints and outward in the plume’s fan.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Figure illustrating various simulated setups of flux emergence evolution over time.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: Radial and tangential Alfvénic and velocity perturbations at r/R ⊙=[1.5, 3, 6, 12] for an emergence rate of 9 G hr–1. Radial Alfvénic perturbations (represented by the blue line) and radial velocity perturbations (represented by the orange line) at various radial locations in the solar corona. The plot also displays the cross helicity (represented by the red and blue color map) at these locations.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: The figure illustrates a jet wisp triggered by magnetic reconnection, where white circles indicate the wisp signatures.
Paper: Modeling the Formation and Evolution of Solar Wind Microstreams: From Coronal Plumes to Propagating Alfvénic Velocity Spikes
Authors: Bahaeddine Gannouni, Victor Réville, Alexis P. Rouillard
Figure caption: The figure illustrates jet expansion during CS evolution.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Time evolution of A 2 of disks with a modified core of different sizes of R  c  and flattening f. All cases start with Q = 2.25.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Surface density map in units of Σ0 for the disk with a modified core of R  c  = 0.5 and f = 0.4 at t = 0 (top panel) and t = 3.03 (bottom panel).
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: Selected regions of the residuals of our fits to the HIRES spectra, compared with log g = 1.5, T eff = 7000 K (green) and T eff = 9000 K (magenta) PHOENIX models. Notice the residual features are consistent with the features seen in these hot model atmospheres, with a tendency for later epochs to more closely resemble the 7000 K atmosphere. This may indicate that the component of the system probed by the residuals is cooling as the disk cools. The HP lines in the lower right panel are strongly affected by Stark broadening in the PHOENIX atmospheres. That we do not see this in the disk model or the data indicates that the contribution from the narrower and weaker HP lines in cooler atmospheres is necessary to match the data.
Paper: Magnetized Accretion Disks with Outflows for Changing-look AGNs
Authors: Wen-Biao Wu, Wei-Min Gu
Figure caption: The accretion timescale of accretion disks at M BH = 108 M ☉ for different α and L bol. The regions of color correspond to the cases for the standard thin disks (blue), magnetically dominated viscous disks (green), and our model (magnetically dominated viscous disks with outflows, yellow). The black dots are the high state (turn-on) of CL-AGNs in Table 1.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The TiO band head at 8860 Å in our models, the HIRES spectra, and the model residuals, shown for all of the HIRES epochs and for three different models. Left: models computed assuming R outer = 12 R ⊙. Notice the time (and therefore ﹩\dot{M}﹩) dependence of the TiO band head is much stronger for this model. Center: models using R outer = 25 R ⊙. Already, there is little change in the TiO band head with time, and it clearly overpredicts the absorptions. Right: models using R outer =45 R ⊙. The TiO band head is essentially insensitive to ﹩\dot{M}﹩ in these models and continues to overestimate the absorption we see.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: Lines in the HIRES spectra which show the central absorption feature shown as a time series progressing from blue to red color. Notice that across the range of lines and EPs, the narrow feature shows a consistent width ∼20 km s−1 and is centered at 0 km s−1. The feature grows as the target fades, absorbing against the disk continuum to additional depth that is almost equivalent to the depth of the disk contribution of many of the lines
Paper: Magnetized Accretion Disks with Outflows for Changing-look AGNs
Authors: Wen-Biao Wu, Wei-Min Gu
Figure caption: Timescales are shown in the ﹩\left\{p,\lambda \right\}﹩-plane for a given L bol/L Edd = 0.05. The dashed line represents ﹩(l=\sqrt{2})﹩ and the solid line corresponds to (l = 2). Each of the color lines corresponds to a specific value on the timescale.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The [O I] λ6300, [N II] λ6583, and [S II] λ6731 emission lines in the HIRES spectra. All three features are blueshifted, with emission components ranging from −60 km s−1 to −10 km s−1. The emission in the [O I] λ6300 and [N II] λ6583 lines is mostly at higher velocities, whereas the [S II] λ6731 line shows both a −40 km s−1 component and a nearly 0 km s−1 component.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The Keplerian velocity at the luminosity-weighted mean radius of each wavelength bin in the outburst spectrum model. Spectral absorption features are visible in the velocity profile because annuli with greater total flux at the slightly greater radii are needed to compensate for the absorption.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: The SFR–stellar mass diagram for our full sample. The red line indicates a linear fit to the field sample only to estimate the star-forming main sequence (SFMS). The average uncertainties in SFR and stellar mass are shown in the top left corner. Above (below) the blue (orange) line represents the “above (below) SFMS” sample that is being used in our analyses. The black dashed line in the horizontal histogram marks the division between low-mass and high-mass samples. Protocluster and field HAEs are distributed similarly in this diagram to illustrate that we are comparing a similar population of galaxies in two different environments.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Each row shows an example of a stacked image (left) and the Sérsic model (middle). The right panels show the residuals of the image. Note that these stacked images are one instance of the bootstrap sampling (Section 4.2).
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: For each sample, we show three randomly selected example HST/ACS F814W 5″ × 5″ cutouts ordered by increasing mass from left to right. We see various apparent morphologies: compact spheroid-like, disky, and irregular or disturbed.