adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Plot of longitude vs. time of all 122 spots modeled for KOI-340, with the markers being sized with respect to the relative radius of the spot group and colored with relative radius as well. The green boxes surrounding each transit correspond to the longitude coverage for each transit. When the green boxes overlap with the next transit, we looked for signs of the spots surviving to the next transit in order to search for signs of differential rotation. An example of this is shown with the overplotted cyan arrow, which encompasses two such instances of possible signs of spots moving in longitude over time.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Top: plot of the surface of KOI-340, with the final spot groups shown as black filled circles, along with the red line denoting the longitude of the star at midtransit and blue lines denoting the full extent of the transit path for the secondary object. Bottom: light curve for final STSP fit (red line) along with the no-spot model for KOI-340 (cyan line) for Transit 21. The residuals (model−data) are shown below the light curve with blue points, with the error bars shown as light-gray lines.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Similar plot to Figure 5, except for Transit 19.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: KOI-340's spot radius distribution is shown in gray with spot radius distributions for typical solar-maximum and solar-minimum sunspots over the same duration as the Kepler mission (4 yr). Here the spot radius is given in relative radius R spot/R * with a bin size width of 0.018 for all three distributions. For comparison, the black dotted vertical lines correspond to the smallest spot (centered around 563.25 BKJD) found in Transit 19 and the main spot (centered at 610.4 BKJD) found in Transit 21 (see Figures 6 and 5), and the red dotted line corresponds to the largest sunspot ever found by Newton (1955) converted to relative radius as shown in Morris et al. (2017).
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: The area of transit crossing chord that is spotted assuming that there are no spots anywhere else on the front hemisphere of KOI-340 is shown as the black distribution. This distribution is then the minimum fractional spotted area for the front hemisphere of KOI-340 compared to the solar-maximum fractional spotted area (red distribution) and solar-minimum fractional spotted area (blue distribution). The solar-maximum and solar-minimum distributions are the same time frames as shown in Figure 10. All three distributions have bin sizes of 0.001 (or 0.1%) fractional spotted area. The y-axis has been broken from 0.4 until 0.9, as the solar-minimum distribution has much smaller fractional spotted areas, so all of the values are in one bin.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Top: plot of the surface of KOI-340, with the final spot groups shown as black filled circles, along with the red line denoting the longitude of the star at midtransit and blue lines denoting the full extent of the transit path for the companion. The red circle denotes the bright spot modeled in this transit. Bottom: light curve for final STSP fit (red line) along with the no-spot model for KOI-340 (cyan line) for Transit 11. The residuals (model–data) are shown below the light curve with blue points.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: The distribution of spot group central longitudes for KOI-340 is shown here in blue. This distribution shows no true peak, meaning that KOI-340 has spots at every longitude equally. As there are no longitudes that are highly favored, it is unlikely that the M-dwarf companion is inducing spots on the surface of KOI-340 that are large enough to be detected over the rotation-induced spots.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: The distribution of spot group central latitudes for KOI-340 is shown here in blue. The distribution is centered at −19.°3, which coincides with where the M-dwarf companion crosses (solid black line). The dashed black lines show the full extent of the secondary crossing path. A total of 24% of the spots fall outside the dotted lines and are thus grazing spots.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Similar plot to both Figures 5 and 6, except for Transit 29.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Original galaxy images and unsharp mask images in the r band of the Fornax dwarf ETG sample. Each image is labeled with the name of the corresponding dwarf galaxy, with its unsharp mask image displayed to its right. The galaxy isophotes at one and two effective radii are overlaid on the original image as red and blue ellipses, respectively. Interloping sources have been masked out. The original images are in units of mag arcsec−2, while the unsharp masks are unitless due to being image ratios. The image scale is shown as a green line, and corresponds to 15″ (1.5 kpc). North is up, east is to the left.
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Heliocentric radial velocity distributions for M31 RGB stars (gray histograms; Section 3.1) in the NE shelf fields. We show the empirical velocity model derived for each field from the 50th percentile values of the marginalized posterior probability distributions (thick red lines; Section 3.2, Table 3). We constructed the velocity models from a kinematically hot halo-like component with fixed mean and standard deviation (thin solid orange lines; Gilbert et al. 2018) and KCCs corresponding predominantly to NE shelf substructure (thin dotted and dashed red lines). We also show the median velocity of the disk predicted for each field assuming its presence (black arrows; Section 3.2.3).
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Similar to Figure 8, except comparing the predictions of N-body models (Fardal et al. 2007, 2012) in the NE shelf region for the formation of the GSS to observations of RGB stars (black points; this work) and PNs (blue open triangles; Merrett et al. 2003, 2006). The models contain a combined bulge, disk, and halo component for the host (orange points) and a satellite component corresponding to GSS-related tidal debris (red points). We show models for a merger remnant with (left panel) and without (right panel) an intact core. The observed projected phase-space distribution of the NE shelf broadly agrees with that of a tidal shell formed from a radial merger with the GSS progenitor, where the model with a completely disrupted progenitor provides a better match (Section 4.2).
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Heliocentric velocity relative to M31's systemic velocity (v M31= −300 km s−1) vs. projected M31-centric radius in the NE shelf fields for stars with successful radial velocity measurements, including both M31 RGB stars (colored points) and MW foreground stars (gray crosses; Section 3.1; left panel) and solely M31 RGB stars color-coded by their kinematically based probability of belonging to substructure (Section 3.2.2; right panel). Velocity errors associated with individual data points are not shown for the sake of clarity (median 5.3 km s−1). The “wedge” pattern visible in this space for M31 RGB stars is characteristic of a tidal shell formed in a radial merger (Section 3.4.1). The right panel also shows the observed upper envelope of the wedge (white open circles; Equation (4)) and its best-fit model (black dotted line, with 1σ confidence interval as gray shaded region; Merrifield & Kuijken 1998) used to place constraints on M31's gravitational potential (Section 3.4.2).
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Photometric metallicity ([Fe/H]phot; top), spectroscopic calcium-triplet-based metallicity ([Fe/H]CaT; middle), and the summed equivalent width of the Na I λ8190 doublet (EWNa; bottom) vs. heliocentric velocity for stars in the NE shelf fields (Table 1) classified as M31 RGB stars (red circles) and MW stars (gray crosses; Section 3.1). Stars in the NE3 velocity peak (Figure 3) are outlined in black. We show [Fe/H]CaT (EWNa) measurements with uncertainties δ[Fe/H]CaT < 0.8 (δEWNa < 2 Å), where the large uncertainties are due to the low spectral S/N. Neither [Fe/H]phot nor [Fe/H]CaT is physically meaningful for MW stars, but they are useful as population diagnostics.
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Similar to Figure 10, except we restricted the selection region for the NE shelf in the N-body models to the location of the spectroscopic fields (Figure 1). Top panels (bottom panels) show the comparison to the M31 host (satellite debris) models with (left panels) and without (right panels) an intact core. The NE shelf region in the simulations is dominated by tidal debris, as opposed to the disk or phase-mixed stellar halo, at the data location, although the models predict a nonnegligible disk contribution from v helio–v M31 ∼ + (50–150) km s−1 at R proj ≲ 23 kpc (Section 4.1).
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Line-of-sight velocity distributions predicted for the NE shelf at the field locations (Figure 11) by N-body models for the formation of the GSS (Fardal et al. 2007, 2012) compared to observations of M31 RGB stars in the NE shelf (see Figure 5). We represent the velocity distributions using Gaussian kernel density estimation with σ = 15 km s−1. We show the predicted velocity distributions for the satellite debris components of the models with (red dotted lines) and without (red dashed lines) an intact core over the radial range spanned by each spectroscopic field. We also show the 1σ confidence intervals (gray shaded regions) from the velocity measurement uncertainty on the observed distributions (solid black lines). Neither model is able to reproduce the velocity distributions in detail, although the model without an intact core is a better match (Section 4.2).
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Photometric metallicity ([Fe/H]phot) distribution functions (MDFs) for all stars in the NE shelf fields (including MW contaminants; black solid open histogram), stars classified as M31 members (gray dashed open histogram; Section 3.1), and stars that probably belong to the NE shelf (p sub > 0.5;  Section 3.2.2). We assumed 12 Gyr PARSEC isochrones (Marigo et al. 2017) to determine [Fe/H]phot (Section 2.2). The median [Fe/H]phot for each sample is shown as arrows, where [Fe/H]phot ,med = −0.41 is robust with respect to sample selection, indicating that the NE shelf is the dominant feature in the data (Section 3.3).
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Heliocentric velocity (v helio) vs. photometric metallicity ([Fe/H]phot) for M31 RGB stars (black points) in the NE shelf fields, where projected M31-centric radius (R proj) increases from left to right and top to bottom. We show the 1σ (2σ) radial velocity range of KCC1 (red) and KCC2 (orange) (Table 3; Figure 5) as dark (light) shaded regions. The [Fe/H]phot distributions across the various NE shelf substructure components are similar. Stars assigned to the stellar halo component also have similar [Fe/H]phot to the NE shelf.
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Histogram of the spatial distribution of satellite debris from the F07 GSS formation model in M31-centric coordinates (Section 4). We show the spectroscopic field locations (colored rectangles) and photometric NE and W shelf edges (black points) from Figure 1 in addition to stream PN candidates (Merrett et al. 2003, 2006). The simulated NE shelf region (black outlined box) is defined using X M31 > 0.2° and −1.5° < Y M31 < 0.5°, where X M31 and Y M31 are defined along the NE major axis (P.A. = 38° E of N) and NW minor axis, respectively.
Paper: Constraining the Size of the Circumgalactic Medium Using the Transverse Autocorrelation Function of C IV Absorbers in Paired Quasar Spectra
Authors: Abby Mintz, Marc Rafelski, Regina A. Jorgenson, Michele Fumagalli, Rajeshwari Dutta, Crystal L. Martin, Elisabeta Lusso, Kate H. R. Rubin, John M. O'Meara
Figure caption: A histogram of DD and RR counts for absorbers in the combined sample as a function of projected separation, normalized by total searchable path length per bin. The three rows show pair counts for velocity widths of δv pair = 500, 200, and 100 km s−1. The empty bars show the the DD pair counts and the solid bars show the RR pair counts. There are significantly more DD pairs than RR pairs for all values of r ⊥ and δv pair. The number of pairs per bin increases as δv pair increases, demonstrating the impact of the velocity width tolerance. We also see that the number of DD counts generally increases with decreasing r ⊥ but begins to flatten at ≈200 h −1 comoving kpc.
Paper: Constraining the Size of the Circumgalactic Medium Using the Transverse Autocorrelation Function of C IV Absorbers in Paired Quasar Spectra
Authors: Abby Mintz, Marc Rafelski, Regina A. Jorgenson, Michele Fumagalli, Rajeshwari Dutta, Crystal L. Martin, Elisabeta Lusso, Kate H. R. Rubin, John M. O'Meara
Figure caption: The transverse autocorrelation function ﹩\xi =\tfrac{{DD}}{{RR}}-1﹩ for the combined sample plotted as a function of perpendicular separation of the quasars pairs for three values of δv pair. As expected, smaller values of δv pair yield higher values of ξ, indicating higher significance of paired absorbers. Following the trend shown in Figure 7, ξ generally increases with decreasing separation. The function begins to level off at ≈200 h −1 comoving kpc. This indicates that the structures we are probing are no smaller than ≈200 h −1 comoving kpc.
Paper: Constraining the Size of the Circumgalactic Medium Using the Transverse Autocorrelation Function of C IV Absorbers in Paired Quasar Spectra
Authors: Abby Mintz, Marc Rafelski, Regina A. Jorgenson, Michele Fumagalli, Rajeshwari Dutta, Crystal L. Martin, Elisabeta Lusso, Kate H. R. Rubin, John M. O'Meara
Figure caption: Equivalent width frequency distributions for W  r,1550 for the absorbers found in the Mintz et al. sample (left) and those found in the Martin et al. sample (right). The black line shows the best-fit line using only the bins plotted in red, which fall between 30 and 500 m Å, chosen to minimize bias from bins with few absorbers. The shaded gray region is the 2σ confidence interval for the best-fit line. The dashed blue line shows the best fit reported in Martin et al. (2010), shown in both plots for comparison. Our calculated frequency distributions agree well with the published results despite slight differences in our methodology.
Paper: Constraining the Size of the Circumgalactic Medium Using the Transverse Autocorrelation Function of C IV Absorbers in Paired Quasar Spectra
Authors: Abby Mintz, Marc Rafelski, Regina A. Jorgenson, Michele Fumagalli, Rajeshwari Dutta, Crystal L. Martin, Elisabeta Lusso, Kate H. R. Rubin, John M. O'Meara
Figure caption: Quasar pairs’ search paths and detected C IV redshifts are shown as a function of pairs’ projected separations. The search path of each pair is plotted using the minimum of the two spectra's lower limits and the maximum of the two quasar's emission redshifts. The stars mark the higher emission redshift of the two quasars in a pair. The C IV absorbers found in the spectra of quasar A of a pair are shown in black and those found in quasar B are shown in red. The pairs from the Mintz et al. sample are plotted in blue, while those from Martin et al. (2010) are plotted in black. The differences in the two samples, including the r ⊥ ranges, redshift ranges, and lengths of the search paths, are clearly visible in this plot.
Paper: Constraining the Size of the Circumgalactic Medium Using the Transverse Autocorrelation Function of C IV Absorbers in Paired Quasar Spectra
Authors: Abby Mintz, Marc Rafelski, Regina A. Jorgenson, Michele Fumagalli, Rajeshwari Dutta, Crystal L. Martin, Elisabeta Lusso, Kate H. R. Rubin, John M. O'Meara
Figure caption: An example of the completeness assessment for J100233.9+353127.5. The upper row shows the completeness in terms of logN, the middle row in terms of W  r,1548, and the bottom row in terms of W  r,1550. The leftmost column shows the completeness fraction as a function of redshift and system strength, with bluer values indicating higher completeness. The middle column shows the total searchable path length in units of δz as a function of logN or W  r . The rightmost column shows the number of injected vs. detected systems in the completeness simulation. Note that the number of injected systems is constant in logN but not in W  r , due to the injection method.
Paper: Constraining the Size of the Circumgalactic Medium Using the Transverse Autocorrelation Function of C IV Absorbers in Paired Quasar Spectra
Authors: Abby Mintz, Marc Rafelski, Regina A. Jorgenson, Michele Fumagalli, Rajeshwari Dutta, Crystal L. Martin, Elisabeta Lusso, Kate H. R. Rubin, John M. O'Meara
Figure caption: A histogram of the W  r,1550 of the final C IV absorber catalog. The W  r,1550 distribution for absorbers from the Mintz et al. sample is shown in a shaded red histogram. The distribution for absorbers from the Martin et al. sample is shown with a dashed blue step histogram. The combined distribution is shown with a black step histogram. Despite the higher S/N of the Martin et al. sample, the two samples have similar lower W  r,1550 detection limits due to the higher resolution of the Mintz et al. sample.
Paper: Constraining the Size of the Circumgalactic Medium Using the Transverse Autocorrelation Function of C IV Absorbers in Paired Quasar Spectra
Authors: Abby Mintz, Marc Rafelski, Regina A. Jorgenson, Michele Fumagalli, Rajeshwari Dutta, Crystal L. Martin, Elisabeta Lusso, Kate H. R. Rubin, John M. O'Meara
Figure caption: Total searchable path in comoving units and completeness percentage are shown as a function of W  r,1550. The functions for the Mintz et al. sample are shown as black solid lines and those for the Martin et al. sample are shown as red dashed lines. Due to the higher emission redshifts of the quasars and the higher S/N of the spectra, the Martin et al. sample has a greater total searchable path and higher completeness for every W  r,1550.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Variation of molecular cloud number, the total angular area, and the total flux with respect to cutoffs. In order to see the distance effects, molecular cloud samples are split into four parts, approximately corresponding to four arm segments (Sun et al. 2021), the Local (−25 to 15 km s−1), the Perseus (−65 to −25 km s−1), the Outer (−95 to −65 km s−1), and the Outer Scutum Centaurus (OSC, −125 to −95 km s−1) arms.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: The area variation of three molecular clouds, G117.7+00.6, G120.3−01.1, and G124.9−01.1, against the cutoffs. Three cases, 10σ, 5σ, and 2σ, are shown for each molecular cloud, and the background images are the integrated maps in the MWISP survey.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Variation of molecular cloud number, the total angular area, and the total flux with respect to the beam size. In order to see the distance effects, molecular cloud samples are split into four parts, approximately corresponding to four arm segments (Sun et al. 2021), the Local (−25 to 15 km s−1), the Perseus (−65 to −25 km s−1), the Outer (−95 to −65 km s−1), and the Outer Scutum Centaurus (OSC, −125 to −95 km s−1) arms.