adsabs/AstroCLIMB huggingface dataset:
Paper: Prediction of Planet Yields by the PRime-focus Infrared Microlensing Experiment Microlensing Survey
Authors: Iona Kondo, Takahiro Sumi, Naoki Koshimoto, Nicholas J. Rattenbury, Daisuke Suzuki, David P. Bennett
Figure caption: Upper panel shows the number of planet detections per dex as a function of the planet mass, M  p . These plots are obtained by integrating over the semimajor axis 0.3 < a < 30 au and over the survey area (8.7–26.2 deg2) shown in Figure 16, assuming the Cassan et al. (2012) mass function as modified by Penny et al. (2019). The red, green, blue, and orange plots show the detection rate for observation strategy S1, S2, S3, and S4 as described in Section 5.1. The pink plot shows the detections when we conduct a spatially uniform survey described in Section 6.1. The lower panel shows the detections of each strategy relative to that of S4.
Paper: The True Nature of the Brightest Local Triple Stellar Candidates within 100 pc in the Galaxy
Authors: Z. T. Yousef, A. Annuar, Mashhoor A. Al-Wardat, N. S. A. Hamid
Figure caption: The positions of the individual components for each stellar system on the evolutionary and isochrone tracks for low- and intermediate-mass stars.
Paper: The True Nature of the Brightest Local Triple Stellar Candidates within 100 pc in the Galaxy
Authors: Z. T. Yousef, A. Annuar, Mashhoor A. Al-Wardat, N. S. A. Hamid
Figure caption: The best-fit synthetic SEDs for the individual components and entire systems studied in this work.
Paper: The True Nature of the Brightest Local Triple Stellar Candidates within 100 pc in the Galaxy
Authors: Z. T. Yousef, A. Annuar, Mashhoor A. Al-Wardat, N. S. A. Hamid
Figure caption: The Mass–Luminosity relation for the systems’ individual components (left) and the entire systems (right), as studied by the Al-Wardat (2002) method between 2002 and 2021.
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: (Left) The 5σ speckle imaging contrast curves in both filters as a function of the angular separation from the diffraction limit (20 mas) out to 1.″2, the end of speckle coherence. The inset shows the reconstructed 562 nm and 832 nm images with a 1″ scale bar. HIP 33609 was found to have no close companions to within the angular and contrast levels achieved. (Middle) Spectral energy distribution of HIP 33609. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black). (Right) The best-fitting MESA Isochrones and Stellar Tracks (MIST) evolutionary track shown in blue with the 3σ contours on the best-fit MIST track in black. The red point indicates the median value and 1σ error bars from our global analysis, while the green contours show the 3σ errors. The blue point indicates the location of 0.5 Gyr on the evolutionary track.
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: The radius evolution of HIP 33609 b. The black point signifies the measured age and radius with 1σ error bars. The orange line is our fiducial evolutionary model (see Section 4.3). The pink line multiplies the atmospheric opacities of the fiducial model by 2, and the red line multiplies the interior metallicity by 5.
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: (Top) The TESS transits for HIP 33609 b phase-folded and binned to 30 minutes. 32 independent draws from the posteriors of the symmetric Mandel & Agol (2002) fit are plotted in orange, and 32 independent draws from the gravity darkening fit (Hooton et al. 2022) are plotted in purple (see Section 4.2). While the median models are very similar betwen the two fits, we note the slight asymmetries seen in the gravity-darkening posteriors hint at a potential misalignment.
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: Color–magnitude diagram (CMD) of stars spatially and kinematically near HIP 33609. The green lines show random draws from our MCMC fit posterior. Points are shaded by the probability that they are part of the outlier model. HIP 33609 is denoted with a red X. The orange and purple lines designate age extremes for reference.
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: Rotation periods of candidate members of MELANGE-6 as a function of B  P  − R  P  color. The rotation periods show a clear sequence as expected for a coeval association, and the outliers tend to be further from HIP 33609 kinematically (see color coding). We show the sequences for Theia 456 (150–200 Myr Andrews et al. 2022) and Pleiades (112 Myr Rebull et al. 2016) for comparison.(The data used to create this figure are available.)
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: The TESS light curves from sectors 6, 8, 33, 34, and 35 extracted using the techniques described in Section 2.1. We note that the gap in flux located at BJD 2459270 is caused by a period of coarse pointing. These poor data were removed in our fit as described in Section 2.1.
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: The TESS and ground-based follow-up transits for HIP 33609 b described in sections Sections 2.1 and  2.2. The model for each transit is shown as a black solid line.
Paper: HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star
Authors: Noah Vowell, Joseph E. Rodriguez, Samuel N. Quinn, George Zhou, Andrew Vanderburg, Andrew W. Mann, Matthew J. Hooton, Keivan G. Stassun, Saburo Howard, Allyson Bieryla, David W. Latham, Steve B. Howell, Tristan Guillot, Carl Ziegler, Karen A. Collins, Theron W. Carmichael, Jon M. Jenkins, Avi Shporer, Lyu ABE, Philippe Bendjoya, Jonathan L. Bush, Marco Buttu, Kevin I. Collins, Jason D. Eastman, Matthew J. Fields, Thomas Gasparetto, Maximilian N. Günther, Veselin B. Kostov, Adam L. Kraus, Kathryn V. Lester, Alan M. Levine, Colin Littlefield, Wenceslas Marie-Sainte, Djamel Mékarnia, Hugh P. Osborn, David Rapetti, George R. Ricker, S. Seager, Ramotholo Sefako, Gregor Srdoc, Olga Suarez, Guillermo Torres, Amaury H. M. J. Triaud, R. Vanderspek, Joshua N. Winn
Figure caption: The radial velocity observations from CHIRON unphased (left) and phased to our best-fit ephemeris (right).
Paper: Disintegration of Long-period Comet C/2021 A1 (Leonard)
Authors: David Jewitt, Yoonyoung Kim, Michael Mattiazzo, Max Mutchler, Jing Li, Jessica Agarwal
Figure caption: Total mass of the debris cloud (assuming density ρ  n  = 500 kg m−3) plotted as a function of the differential power-law index, γ, as a solid black line. The equivalent spherical mass of the original nucleus of 0.6 ± 0.2 km radius is shown (assuming the same ρ  n ), together with its uncertainty, as a yellow horizontal band. The masses of the debris and nucleus are equal at γ  =  3.5 ± 0.1, shown by the red filled circle. For comparison we show, as a blue square, the size distribution of the Kreutz sungrazing comets (Knight et al. 2010) and, as green triangles, several radar-measured meteoroid streams (Blaauw et al. 2011). The vertical positions of the points for the Kreutz and radar stream have no meaning.
Paper: Disintegration of Long-period Comet C/2021 A1 (Leonard)
Authors: David Jewitt, Yoonyoung Kim, Michael Mattiazzo, Max Mutchler, Jing Li, Jessica Agarwal
Figure caption: (A) Composite of four, 450 s HST images from UT 2022 April 5. Diffuse streaks are imperfectly removed field stars and galaxies. (B) Same image, annotated to show the approximate boundary of the debris (white dashed line) and the expected location of the nucleus (yellow line segments). Two scale bars of 30″ and 5 × 104 km in length are shown, as well as the projected antisolar (−S) and negative heliocentric velocity (−V) vectors. North is to the top, east to the left.
Paper: Disintegration of Long-period Comet C/2021 A1 (Leonard)
Authors: David Jewitt, Yoonyoung Kim, Michael Mattiazzo, Max Mutchler, Jing Li, Jessica Agarwal
Figure caption: Top: same image as in Figure 2 but rotated to bring the axis of the dust tail to the horizontal and shown on a larger scale. Yellow lines mark the ephemeris location of the nucleus. Bottom: locations of the photometry regions A, B, and C used to measure the scattering cross section of particles in the tail.
Paper: Disintegration of Long-period Comet C/2021 A1 (Leonard)
Authors: David Jewitt, Yoonyoung Kim, Michael Mattiazzo, Max Mutchler, Jing Li, Jessica Agarwal
Figure caption: Wide-field image from Swan Hill Observatory showing C/2021 A1 on UT 2022 March 31. 10′ and 106 km scale bars are shown, as well as the projected antisolar (−S) and negative heliocentric velocity (−V) vectors. Yellow lines mark the ephemeris location of the nucleus. The white square shows the size of the HST field of view. The image has north to the top, east to the left.
Paper: Disintegration of Long-period Comet C/2021 A1 (Leonard)
Authors: David Jewitt, Yoonyoung Kim, Michael Mattiazzo, Max Mutchler, Jing Li, Jessica Agarwal
Figure caption: Left: the same image as Figure 2 with synchrones overplotted, for ejection dates 80, 100, 120, 140, and 160 days prior to the date of the image. Right: syndynes for particles with β = 0.0003, 0.001, 0.003, 0.01, and 0.03, as marked. The axis of the debris cloud is best matched by the synchrones for 110 ± 10 days, corresponding to ejection on UT 2021 December 11 ± 10.
Paper: Disintegration of Long-period Comet C/2021 A1 (Leonard)
Authors: David Jewitt, Yoonyoung Kim, Michael Mattiazzo, Max Mutchler, Jing Li, Jessica Agarwal
Figure caption: Surface brightness profile parallel to the long axis of Box A (Figure 3) plotted against the distance from the ephemeris location of the nucleus (axis is reversed relative to Figure 3). 1000 units correspond to a surface brightness Σ = 24.4 mag arcsec−2. The linear distance scale is approximately 1500 km per arcsecond.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: (a) Zoom in on 50 day portion of KIC 5024084’s light curve. (b) Low-frequency portion of KIC 5024084 amplitude spectrum, showing many low-frequency modes. (c) Zoom in on low amplitudes of KIC 5024084 amplitude spectrum, with frequency range extended to 12 c/d. A single 11.2 c/d mode is visible in δ Sct frequency range.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: (a) KIC 5113357’s amplitude spectrum, extended to 50 c/d. Some frequencies above the Nyquist frequency of 24.4695 c/d have higher amplitudes than their reflections and are real frequencies. (b) Zoom in on the low-amplitude and low-frequency portion of KIC 5113357’s amplitude spectrum. A few low-amplitude frequencies are present in the γ Dor frequency range.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: (a) Zoom in on a five day portion of KIC 5024468’s light curve. (b) Amplitude spectrum for KIC 5024468 showing δ Sct modes. The Nyquist frequency for the 30 minute cadence Kepler data is 24.4695 c/d, but the spectrum extends to 28 cycles/day as there are real super-Nyquist frequencies that have higher amplitudes than their reflections. (c) Zoom in on the low-amplitude portion of KIC 5024468 spectrum showing many significant low-amplitude modes in both the γ Dor and δ Sct frequency ranges.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: (a) Zoom in on a five day portion of the light curve of the eclipsing binary KIC 5024450, showing eclipses with a period of 3.05 days. This light curve is contaminating the light curve of 5024468, and the binary orbital frequency and its harmonics were removed when determining the frequencies of KIC 5024468 in Table A.1. (b) Amplitude spectrum of KIC 5024450, showing the characteristic comb-like pattern of an eclipsing binary. The δ Sct oscillations of KIC 5024468 around 12 c/d also contaminate the KIC 5024450 spectrum.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: (a) Zoom in on a 10 day portion of KIC 5113357’s light curve. (b) Zoom in on two day portion of KIC 5113357’s light curve.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: (a) A five day zoom in on KIC 5112843’s light curve. The dominant property is two close frequencies beating against other. (b) KIC 5112843’s amplitude spectrum.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: (a) Zoom in on a 20 day portion of KIC 5024455’s light curve. (b) KIC 5024455 amplitude spectrum.
Paper: Disintegration of Long-period Comet C/2021 A1 (Leonard)
Authors: David Jewitt, Yoonyoung Kim, Michael Mattiazzo, Max Mutchler, Jing Li, Jessica Agarwal
Figure caption: Axial surface brightness profile on UT 2022 March 31 (yellow diamonds) compared with results from a Monte Carlo simulation. The models shown have size index γ = 3.3 (red curve), 3.4 (black curve), and 3.5 (blue curve), all with 7 × 10−4 ≤ β ≤ 0.07, corresponding to particle radii of 14 μm–1.4 mm.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: Spacing between consecutive periods vs. period for KIC 5024084 (a) and KIC 5024455 (b) resulting from further prewhitening of the light curve to identify additional low frequencies. The points in light blue or red represent hypothetical spacing sequences. The lines show linear regression fits to these sequences.
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: K-S test results for the frequency separations of the δ Sct stars KIC 5024468 (a) and KIC 5113357 (b).
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: Spacing between consecutive periods vs. period for the γ Dor candidates KIC 5024084 (a) and KIC 5024455 (b).
Paper: Variable Blue Straggler Stars in the Open Cluster NGC 6819 Observed in the Kepler “Superstamp” Field
Authors: Joyce A. Guzik, Andrzej S. Baran, Sachu Sanjayan, Péter Németh, Anne M. Hedlund, Jason Jackiewicz, Lori R. Dauelsberg
Figure caption: Distribution of frequency spacings for the δ Sct stars KIC 5024468 (a) and KIC 5113357 (b).
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The velocity-integrated intensity images of the 12CO (top panel) and 13CO (bottom panel) emission toward the Galactic Cassiopeia region. The unit of the scale bar is K km s−1. In the 12CO image, the blue line shows the main filament identified by the DisPerSE algorithm (named after the Cassiopeia Filament in this work), while the orange lines show the identified subfilaments. In the 13CO image, the blue dashed-line rectangle marks the extent of the giant arc-like shell.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: (a) The excitation temperature image of the observed Cassiopeia region. The unit of the scale bar is K. (b) The H2 column density image derived from the 13CO data within the velocity range of [+1, +4] km s−1, assuming the LTE condition. The unit of the scale bar is 1021 cm−2. (c) The H2 column density image derived from the 12 CO data within the velocity range of [+1, +4] km s−1, adopting the CO-to-H2 conversion factor. The unit of the scale bar is 1021 cm−2.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: (a) The measured distance toward the filament’s east end. The middle panel shows the MWISP 12CO intensity image. The green contour shows the edge of the molecular cloud (3σ threshold), while green and blue dots represent on- and off-cloud Gaia DR2 stars. In the top right panel, green and blue points represent on- and off-cloud stars (binned every 5 pc), respectively. The dashed red line is the modeled extinction A  V . The distance is derived with raw on-cloud Gaia DR2 stars, which are represented with gray points. The black vertical lines indicate the distance (D) estimated with Bayesian analyses and Markov Chain Monte Carlo (MCMC) sampling, and the shadow area depicts the 95% highest posterior density (HPD) distance range. The corner plots of the MCMC samples are displayed in the left panel (distance, the extinction of foreground and background stars and uncertainties). The mean and 95% HPD of the samples are shown with solid and dashed vertical lines, respectively. (b) The measured distance toward the west shell, and Gaia G-band data are used.