adsabs/AstroCLIMB huggingface dataset:
Paper: A Novel Test for MOND: Gravitational Lensing by Disk Galaxies
Authors: Christopher Harvey-Hawes, Marco Galoppo
Figure caption: Lensing configuration for SGL by a disk galaxy. We report source, lens, and observer positions, as well as the relevant angles and coordinate systems. Here, α is the deflection angle, β is the angular source position, and θ is the angular image position.
Paper: A Novel Test for MOND: Gravitational Lensing by Disk Galaxies
Authors: Christopher Harvey-Hawes, Marco Galoppo
Figure caption: Ratio of the baryon density to the PDM density, ρB/ρph, along the radial direction on the equatorial plane (top panel), and the corresponding two-dimensional distribution in the x–z plane within a scale height of the galactic disk (bottom panel) for a disk galaxy with Md = 1011 M⊙, Rd = 3.5 kpc, zd = 0.35 kpc, Mb = 109 M⊙, and rb = 0.7 kpc. The purple dashed line in the top panel highlights the point at which the two densities have the same value. The interpolating function employed here refers to that of Equation (21).
Paper: A Novel Test for MOND: Gravitational Lensing by Disk Galaxies
Authors: Christopher Harvey-Hawes, Marco Galoppo
Figure caption: PDM density distribution, for the interpolating function of Equation (21), on the x–z plane (upper panel) and on the x–y plane (lower panel) for a disk galaxy with Md = 1011 M⊙, Rd = 3.5 kpc, zd = 0.35 kpc, Mb = 109 M⊙, and rb = 0.7 kpc. A log scale is used for the density to highlight the morphology of the PDM distribution.
Paper: A Novel Test for MOND: Gravitational Lensing by Disk Galaxies
Authors: Christopher Harvey-Hawes, Marco Galoppo
Figure caption: Example of lensing observables, namely the deflection angle (α), the magnification (μ), and the shear (γ), for a disk galaxy of inclinations i = 0 (left) and i = π/2 (right). The disk galaxy model is obtained by fixing Md = 1011 M⊙, Rd = 3.5 kpc, zd = 0.35 kpc, Mb = 109 M⊙, and rb = 0.7 kpc, and applying the interpolating function of Equation (21).
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: Baryon content as a function of halo mass across the three CAMELS models. Each row focuses on a specific model (TNG, SIMBA, and ASTRID, respectively), while each column focuses on the effect of varying a single feedback parameter (ASN1, ASN2, AAGN1, and AAGN2, respectively). Thick solid lines show a running mean of the total baryon content as a function of halo mass across the CAMELS LH runs, and thin dashed lines show the fraction of baryons in stars. The baryon content shows how the amount of gas in the ISM and CGM of the halo is affected by varying feedback, and higher fbaryon generally correlates with larger SFH widths and more efficient baryon cycling.
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: Similar to Figure 9, but for the relative mass of the central SMBH as a function of halo mass across the three simulations while varying feedback. Black holes in ASTRID are generally more massive at z ∼ 0 compared to the other models, and are correlated with the earlier quenching observed in their SFHs.
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: Similar to Figure 9, but for the ratio of stellar to gas mass across the three simulations while varying feedback. The change in the stellar-to-gas mass ratio compared to the baryon fraction traces the star formation efficiency compared to the overall amount of baryons in the ISM and CGM of the halo.
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: Top: summary of the various factors impacting average galaxy SFHs across the three CAMELS models. Bottom: feature importance of the cosmology, feedback scaling factors, and galaxy properties as defined in Equation (18) on the SFR as a function of lookback time. Cosmology dominates the average SFR of galaxies at early times, giving way to halo mass as they assemble. At late times, the SFR is a complex interplay of feedback and baryon cycling. This behavior generalizes across the three models, but the relative contributions differ.
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: The frequency with which different terms occur in the symbolic regression solutions to the SFH parameters across the three CAMELS models. While different from traditional metrics of feature importance (e.g., using saliency maps or random forests), the occurrence of certain recurring terms (e.g., Mhalo being an important feature for ϕ across all three models) in the set of equations generated by symbolic regression aid in the construction of equations that generalize across the CAMELS models.
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: Changes in the SFHs for all three CAMELS models while varying ASN1 and ASN2 such that the energy per unit SFR is varied while keeping the mass loading factor fixed, at low (top), intermediate (middle), and high (bottom row) halo masses (using the normalizing-flow emulator developed in Section 3.1). Note that (except for the high-mass halos where black hole feedback dominates), increasing the energy per unit SFR (at fixed mass loading η) leads to less star formation.
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: Varying the energy per unit SFR (ASN1) and wind speed (ASN2) in CAMELS/TNG have distinct effects on the baryon fraction and stellar-to-gas mass ratio. This allows us to disentangle the effects of factors that change the gas content of halos from factors that change the efficiency of forming stars from that gas. The black lines show lines of constant baryon fraction to stellar-to-gas mass ratio. While increasing ASN1 changes the star formation efficiency, changing ASN2 tends to affect the baryon content of the halo.
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: Variations in the baryon fraction (top panels) and black hole mass (bottom panels) for all three simulations (from left to right: CAMELS/TNG, CAMELS/SIMBA, and CAMELS/ASTRID) as a function of halo mass. Within each set of six panels, the top column shows the result of varying the mass loading while keeping the energy per SFR constant while the bottom column is the opposite.
Paper: How Does Feedback Affect the Star Formation Histories of Galaxies?
Authors: Kartheik G. Iyer, Tjitske K. Starkenburg, Greg L. Bryan, Rachel S. Somerville, Juan Pablo Alfonzo, Daniel Anglés-Alcázar, Suchetha Cooray, Romeel Davé, Austen Gabrielpillai, Shy Genel, Sultan Hassan, Lars Hernquist, Christian Kragh Jespersen, Christopher C. Lovell, Boon Kiat Oh, Camilla Pacifici, Lucia A. Perez, Laura Sommovigo, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Megan T. Tillman, Francisco Villaescusa-Navarro, John F. Wu
Figure caption: Same as Figure 14 but now varying the mass loading η while keeping the energy per star formation constant. Note that (except at very early times) increasing the mass loading of galactic winds actually leads to more star formation.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: nVF at different energy bands for a sinusoidal wave (source g3; Equation (7)), cases 15–18 (Table 1)). Continuous lines show results for τacc =  5 s, dashed lines show results for τacc =  25 s. The left column displays results for n = 3 × 1010 cm−3, while the right column shows results for n = 5 × 109 cm−3.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: Spectral index at different energy bands for a sinusoidal wave (source g3; Equation (7)) for cases 15–18 (Table 1). Continuous lines show results for τacc = 5 s, dashed lines show results for τacc = 25 s. The left column displays results for n = 3 × 1010 cm−3, while the right column shows results for n = 5 × 109 cm−3. δnVF was computed using data from Figure 7.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: nVF at different energy bands for a square pulse (source g2; Equation (6)), where turbulent acceleration turns on at t =  10 s and turns off at t =  30 s. Continuous lines show results for τacc =  5 s, dashed lines show results for τacc =  25 s. The left column displays results for n = 3 × 1010 cm−3, while the right column shows results for n = 5 × 109 cm−3.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: Panels (a) and (c) show the response timescale, τon, and panels (b) and (d) the response timescale, τoff, measured at the loop top for cases 5–14 (Table 1). Continuous lines represent the response timescale measured from Figure 5(c) and (d). Dashed lines represent the exponential fits described in Equation (24) and Figure 15 in Appendix B.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: nVF at different energy bands for a damped wave (source g4; Equation (8)). Continuous lines show results for τacc =  5 s, dashed lines show results for τacc =  25 s. The left column displays results for n = 3 × 1010 cm−3, while the right column shows results for n = 5 × 109 cm−3.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: nVF (blue) measured for the full flare and g4 (orange) for simulation case 22, where τacc =  25 s, n = 5 × 109 cm−3.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: Response timescale (Equation (26)) computed for a sinusoidal wave (source g3; Equation (7)) obtained from the nVF time series shown in Figure 7. Panels (a) and (c) contain results for higher plasma number density, and panels (b) and (c) for lower plasma number density. The dashed lines represent a fit using an exponential function (Equation (24)).
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: Normalized damping envelope, ﹩\exp [-(t-15)/{\tau }_{{\rm{\exp }}}]﹩, for nVF time series extracted from Figure 11, for simulation cases 19–22 in Table 1.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: nVF (blue) measured for the full flare and g3 (orange) for simulation case 18 (Table 1), where τacc =  25 s, n = 5 × 109 cm−3.
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: Surface brightness profile of NGC 6166. Data obtained from B. T. Dullo (2019).
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: Cumulative areal event rate of second-timescale glints as a function of magnitude (0.5 s equivalent). For our survey with Tomo-e Gozen, the average rate (blue) and the rate near the equator (red, −20° < decl. < +20°) are shown. Event rates estimated with Evryscope (H. Corbett et al. 2020), W-FAST (G. Nir et al. 2021a), and ZTF (S. Karpov & J. Peloton 2023) are also shown for comparison (see Table 1). The magnitude range for Evryscope (120 s exposure time) and ZTF (30 s exposure time) is converted to 0.5 s equivalent magnitude. The magnitude range for W-FAST (0.04 exposure time, resolving the glint light curves) is also converted by assuming a typical intrinsic duration of the glints Δt = 0.2 s. The ZTF rate shown in this figure is the rate for all the candidates, including uncataloged sources. To estimate the foreground rate for the future surveys, all the event rates in this figure are defined in a detection-wise way: multiple glints from the same objects are counted multiple times.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: (Top) Brightness distribution for the glints that are not matched with cataloged objects. (Bottom) The relation between the magnitude and the size of the objects. The purple solid line shows the expected size assuming an albedo of A = 0.175 and scattered reflection with the phase angle of ϕ = 90° at the GEO. The purple dashed line shows a smaller size by a factor of 10 to give a possible range. The black line shows the expected size assuming a perfect mirror reflection with albedo of A = 0.175. The gray dots show the size estimated from radar cross section (﹩l=\sqrt{{\rm{RCS}}}﹩) for the glints associated with cataloged objects with an apogee of >30,000 km.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: Magnitude distribution of the detected glints (blue). (Top) Gray line shows the magnitudes of the glints detected in images deeper than 16.5 mag, which is used for the event rate estimate. The magnitude distribution of the glints associated with cataloged objects is shown with the orange line. (Bottom) The distributions of the glints with single and multiple detections are shown with the black and green lines, respectively. Note that magnitudes are given as measured in the 0.5 s image.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: Precision–recall curve of our detection algorithm. Two large dots show the precision and recall with a threshold score of 0.35 and 0.70. Small dots are given with an interval of 0.01 in the threshold score. A jump in a high recall with the lowest threshold score is due to the very faint artificial sources, which are always difficult to detect (see Figure 3).
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: Apparent motion in R.A. and decl. for the glints detected ≥three times (blue). The orange dots show the motions of the objects associated with cataloged objects. The gray dots show the motions of the objects at decl. >20°.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: Example of detected glints. For the glints matched with cataloged objects, their common names are also given. Each image section has a size of 100 pixels × 100 pixels (about 2′​​​​​​ × 2′). North is up and east is left. Note that some faint sources (i.e., those in SIRIUS 3 (first row), uncataloged source (fourth row), and HIMAWARI 5 AKM (fifth row)) are not detected with SSD, and these are not included in the number of detections.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: Distribution of solar separation angles for the detected glints (blue). For comparison, the gray line shows the (normalized) angle distribution for our survey footprints. The thin dashed line shows the uniform distribution.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: Example of training data for the SSD: stationary source (top), transient (middle), and background (bottom). Three images for each category show three consecutive time frames.
Paper: Dynamical Masses for 23 Pre-main-sequence Stars in Upper Scorpius: A Critical Test of Stellar Evolutionary Models
Authors: A. P. M. Towner, J. A. Eisner, P. D. Sheehan, L. A. Hillenbrand, Y.-L. Wu
Figure caption: 12CO intensity-weighted velocity (moment 1) maps for all 25 targets. All panels are in ICRS coordinates, with a 4″ field of view. All color bars are in kilometers per second, and are centered on a VLSR determined from a by-eye examination of each target’s spectrum. Each image is masked such that only pixels with (a) a S/N > 2σ in (b) at least two consecutive channels and (c) at least 4 pixels square are included in the moment maps. The 0.5 × Ipeak continuum contours are overlaid in black. The 12CO beam is shown in the bottom left of each panel, the continuum beam in the bottom right, and an angular and physical scale bar in the top center.
Paper: Dynamical Masses for 23 Pre-main-sequence Stars in Upper Scorpius: A Critical Test of Stellar Evolutionary Models
Authors: A. P. M. Towner, J. A. Eisner, P. D. Sheehan, L. A. Hillenbrand, Y.-L. Wu
Figure caption: 345 GHz continuum images for all 25 targets in the sample. All panels are in ICRS coordinates, with a field of view of 2″. All color bars are in units of millijanskys per beam−1. The 0.5 × Ipeak contour for each source is shown as a black dashed line. The continuum beam for each field is shown in the bottom-left corner of each image, and an angular and physical scale bar in the top center. Source J15562477−2225552 is a nondetection at 3σ.
Paper: Dynamical Masses for 23 Pre-main-sequence Stars in Upper Scorpius: A Critical Test of Stellar Evolutionary Models
Authors: A. P. M. Towner, J. A. Eisner, P. D. Sheehan, L. A. Hillenbrand, Y.-L. Wu
Figure caption: As in Figure 2, but for 13CO emission. Only sources with 13CO detections are shown.