adsabs/AstroCLIMB huggingface dataset:
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: Attenuation maps (Aλ; left side) and their respective uncertainties (ΔAλ; right side). Top row: attenuation calculated from the HST F606W filter, whose reference wavelength is 0.606 μm. Middle row: attenuation calculated from the JWST F090W filter, whose reference wavelength is 0.90 μm. Bottom row: attenuation calculated from the JWST F150W filter, whose reference wavelength is 1.50 μm. All maps are overlaid (green for Aλ and white for ΔAλ) with their respective S/N maps (that is, the HST F606W and JWST F090W and F150W filters each have their own S/N maps, not given in this paper) as a contour such that S/Nλ ≥ 1. All contour maps are smoothed over (3 pixels across). Also overlaid in black is the Petrosian radius (RP =  12 kpc). These attenuation structures are well outside the stellar disk.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: Ratio of total to selective attenuation (﹩{R}_{\widetilde{VI}}﹩; left) map approximated via Monte Carlo resampling of n = 1000 iterations and its resulting standard error of the distribution mean (right). ﹩{R}_{\widetilde{VI}}﹩ is simply calculated from Equation (1).
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: AV, ﹩{R}_{\widetilde{VI}}﹩, and α maps shown of three regions of contrasting environments in the outskirts of VV 191b that are well backlit by the foreground galaxy, VV 191a. The maps are zoomed in to the three regions to be analyzed at small scales. Region A (red) closely resembles a dense spiral arm. Region B (green) is a less dense tendril branch to a spiral arm. Region C (blue) is on the edge or possibly outside of the galaxy disk.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: A red, green, and blue (RGB) image of overlapping galaxy pair VV 191. Red and green are the NIRCam F150W and F090W filters, respectively. Blue is the HST F606W filter. The galaxy pair consists of a foreground spiral Sc galaxy, VV 191b, and a smooth background elliptical galaxy, VV 191a. The redshifts for the foreground and background galaxies are z = 0.0514 and z = 0.0513, respectively. The area of overlap shown in Figures 3–5 is overlaid in white. Small regions of high S/N, A, B, and C (see Section 5.3), are overlaid and labeled in red, blue, and green, respectively. In addition, the best background elliptical model is overlaid in dotted gray to display the extent of the background elliptical galaxy.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: Left: the reddening slope ﹩{R}_{\widetilde{VI}}﹩ plotted against AV throughout all pixels that meet the criteria mentioned in Section 4.2. Right: the NIR attenuation power-law index α plotted against AV. Both plots are two-dimensional hexagonal-binned histogram density plots. To ensure high confidence that the reported pixels are sufficiently backlit by the background galaxy, additional thresholds for the galactocentric radius, R ≥ 8 kpc, and AV, AF090W ≥ 0, are imposed.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: SED for an elliptical galaxy (black) and the filter throughput for each of the five broadband filters used in the approximation of α. The filter throughputs can be found from the SVO Filter Profile Service (https://svo2.cab.inta-csic.es/theory/fps).
Paper: Classifying Compact Radio Emission in Nearby Galaxies: A 10 GHz Study of Active Galactic Nuclei, Supernovae, Anomalous Microwave Emission, and Star-forming Regions
Authors: Kristen C. Dage, Eric W. Koch, Evangelia Tremou, Kwangmin Oh, Susmita Sett, Cosima Eibensteiner, Sean T. Linden, Angiraben D. Mahida, Eric J. Murphy, Muhammad Ridha Aldhalemi, Zainab Bustani, Mariam Ismail Fawaz, Hans J. Harff, Amna Khalyleh, Timothy McBride, Jesse Mason, Anthony Preston, Cortney Rinehart, Ethan Vinson, Teresa Panurach, Richard M. Plotkin, Liliana Rivera Sandoval
Figure caption: HST Hα imaging of M51 with the location of Source 65 from L. A. Maddox et al. (2007) at 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 and our X-band detection (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15). The coincidence with a compact Hα source and the steep spectrum of α = 2.7 ± 0.1 suggests the source may be a radio-opaque and compact HII region.
Paper: Classifying Compact Radio Emission in Nearby Galaxies: A 10 GHz Study of Active Galactic Nuclei, Supernovae, Anomalous Microwave Emission, and Star-forming Regions
Authors: Kristen C. Dage, Eric W. Koch, Evangelia Tremou, Kwangmin Oh, Susmita Sett, Cosima Eibensteiner, Sean T. Linden, Angiraben D. Mahida, Eric J. Murphy, Muhammad Ridha Aldhalemi, Zainab Bustani, Mariam Ismail Fawaz, Hans J. Harff, Amna Khalyleh, Timothy McBride, Jesse Mason, Anthony Preston, Cortney Rinehart, Ethan Vinson, Teresa Panurach, Richard M. Plotkin, Liliana Rivera Sandoval
Figure caption: Our resolved observations reveal clear AGN jets at position 12:42:03.59 +32:32:16.28 within the NGC 4631 field, strongly suggesting this is a background radio-bright AGN. However, this source has previously been cataloged as a SFR based on lower resolution radio SED modeling by S. T. Linden et al. (2020), and as a HMXB from the coincident X-ray emission by S. Mineo et al. (2012). The orange band contours show 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩8 diffuse S-band emission at 0.3, 0.6, and 2 mJy (S. T. Linden et al. 2020). Our finding emphasizes the need for resolved radio surveys to distinguish sources within the host and background objects.
Paper: Classifying Compact Radio Emission in Nearby Galaxies: A 10 GHz Study of Active Galactic Nuclei, Supernovae, Anomalous Microwave Emission, and Star-forming Regions
Authors: Kristen C. Dage, Eric W. Koch, Evangelia Tremou, Kwangmin Oh, Susmita Sett, Cosima Eibensteiner, Sean T. Linden, Angiraben D. Mahida, Eric J. Murphy, Muhammad Ridha Aldhalemi, Zainab Bustani, Mariam Ismail Fawaz, Hans J. Harff, Amna Khalyleh, Timothy McBride, Jesse Mason, Anthony Preston, Cortney Rinehart, Ethan Vinson, Teresa Panurach, Richard M. Plotkin, Liliana Rivera Sandoval
Figure caption: Location of X-band radio sources in M51 that match with archival multiband radio sources (S. T. Linden et al. 2020) or Chandra X-ray detections overlaid on DSS2 imaging. The SFRs and AME classifications come from S. T. Linden et al. (2020).
Paper: Classifying Compact Radio Emission in Nearby Galaxies: A 10 GHz Study of Active Galactic Nuclei, Supernovae, Anomalous Microwave Emission, and Star-forming Regions
Authors: Kristen C. Dage, Eric W. Koch, Evangelia Tremou, Kwangmin Oh, Susmita Sett, Cosima Eibensteiner, Sean T. Linden, Angiraben D. Mahida, Eric J. Murphy, Muhammad Ridha Aldhalemi, Zainab Bustani, Mariam Ismail Fawaz, Hans J. Harff, Amna Khalyleh, Timothy McBride, Jesse Mason, Anthony Preston, Cortney Rinehart, Ethan Vinson, Teresa Panurach, Richard M. Plotkin, Liliana Rivera Sandoval
Figure caption: Our three targeted galaxies and their locations relative to the z = 0 massive galaxy populations from z0MGS (A. K. Leroy et al. 2019). Though a small sample, we highlight that all of these sources lie close to the locus of star-forming main-sequence galaxies.
Paper: Classifying Compact Radio Emission in Nearby Galaxies: A 10 GHz Study of Active Galactic Nuclei, Supernovae, Anomalous Microwave Emission, and Star-forming Regions
Authors: Kristen C. Dage, Eric W. Koch, Evangelia Tremou, Kwangmin Oh, Susmita Sett, Cosima Eibensteiner, Sean T. Linden, Angiraben D. Mahida, Eric J. Murphy, Muhammad Ridha Aldhalemi, Zainab Bustani, Mariam Ismail Fawaz, Hans J. Harff, Amna Khalyleh, Timothy McBride, Jesse Mason, Anthony Preston, Cortney Rinehart, Ethan Vinson, Teresa Panurach, Richard M. Plotkin, Liliana Rivera Sandoval
Figure caption: As in Figure 4 for NGC 4631. Our work identifies the AGN based on the resolved radio lobe morphology (see Section 3.2); this source was previously classified as a SFR in S. T. Linden et al. (2020) and a HMXB by S. Mineo et al. (2012).
Paper: Classifying Compact Radio Emission in Nearby Galaxies: A 10 GHz Study of Active Galactic Nuclei, Supernovae, Anomalous Microwave Emission, and Star-forming Regions
Authors: Kristen C. Dage, Eric W. Koch, Evangelia Tremou, Kwangmin Oh, Susmita Sett, Cosima Eibensteiner, Sean T. Linden, Angiraben D. Mahida, Eric J. Murphy, Muhammad Ridha Aldhalemi, Zainab Bustani, Mariam Ismail Fawaz, Hans J. Harff, Amna Khalyleh, Timothy McBride, Jesse Mason, Anthony Preston, Cortney Rinehart, Ethan Vinson, Teresa Panurach, Richard M. Plotkin, Liliana Rivera Sandoval
Figure caption: As in Figure 4 for NGC 5474, with position N1 marking the background galaxy.
Paper: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory
Authors: Katie E. Painter, Brendan P. Bowler, Kyle Franson, Juliette C. Becker, Jennifer A. Burt
Figure caption: Companion mass vs. separation for all targets in the HGCA as shown in Figure 2. Planets are plotted as green circles and stellar, white dwarf, brown dwarf companions as yellow stars. The light gray region at the top of each plot defines the mass range greater than the mass of the host star. 1σ errors are shown for the masses of the planets and the separations of all the companions. A companion is consistent with the acceleration if these errors overlap with the 2σ confidence interval derived from the astrometry. Note that some companions are outside of the bounds of these plots, and thus not shown, but they do not account for the acceleration in any of these cases. (Download all images (tar.gz).)
Paper: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory
Authors: Katie E. Painter, Brendan P. Bowler, Kyle Franson, Juliette C. Becker, Jennifer A. Burt
Figure caption: Left: dynamical stability analysis of HZs. Known planets (green circles) and companions in the stellar/brown dwarf mass range (yellow stars) are shown relative to the region of physical instability for an Earth-mass planet situated in the HZ (gray contours). The separations are normalized to the center of the HZ in each system. The stability limits are calculated per B. Quarles et al. (2018, 2020) above 1 MJup (dotted line) and using the Hill stability criterion below. The dashed–dotted line delineates the stellar–brown dwarf boundary and the dashed line delineates the brown dwarf–planet boundary. The dark gray shading represents the region where a second companion in the system would cause an Earth-mass planet located directly in the middle of the HZ to be unstable. The medium gray shading represents the region where a companion would threaten an Earth-mass planet in some part of the CHZ. The light gray shading represents the region where a companion would threaten an Earth-mass planet in some portion of the OHZ. Note that the cyan star is attributed to a spectroscopic binary in the τ1 Eridani system detailed in Section 4.1. Right: constraints on systems with accelerations from previously unknown companions. The same instability contours are shown along with the mass–separation curves for the 17 unaccounted-for accelerations.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Panel A: fractional difference between planet radii from asteroseismology and those from V. Van Eylen et al. (2018; VE18): (Rp, this work − Rp, VE18)/Rp, VE18. Panel B: planet radii on period–radius plane, where the gray and blue points are planet radii from VE18 and asteroseismology, respectively, and the dashed line indicates the radius valley, with best-fit parameters (m = −0.09 and α = 0.37) and axes limits from VE18. Panel C: distribution of planet radii from asteroseismology (blue), and from VE18 (dashed black).
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Kepler stars for which we did not find solar-like oscillations in DR25, but were previously classified as detections. Each subpanel shows the power spectrum of the target, centered on the expected νmax as indicated by the red dashed line.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Panel A: comparing the distribution of white noise and Kepler apparent magnitude (Kp) between detections (blue points) and nondetections (unfilled). Panel B: same as Panel A, but investigating white noise as a function of the length of the time series. Panel C: same as Panel A, but investigating white noise as a function of detection probability.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Smoothed and background-corrected power spectra for 25 of the 50 new detections as found by pySYD, centered on νmax.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Same as Figure A1, for the other 25 of the 50 new detections found in this work.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Rotation periods as a function of effective temperatures for all detections (unfilled points), including new detections (blue), planet hosts (yellow), and new planet hosts (orange). The complete sample from A. R. G. Santos et al. (2021) is shown for reference as a density distribution.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Left panel: phase coverage of WASP-189 b’s orbit during our two observing nights. The orbit of WASP-189 b is shown face-on (dotted black line), with the observer’s direction indicated. Relative orbital phases (ϕ) are annotated along quarterly intervals. The first (green) and second (wine red) nights cover the pre-eclipse and post-eclipse phases. Both nights cover (part of) the secondary eclipse. Right panel: time series of three observables: the signal-to-noise rate per frame pair (S/N), FWHM of the trace on the detector (in pixels), and airmass are shown. The same colors as in the left panel are used to indicate each night. The time series has been binned (10 frames per bin), and the standard deviation of each bin is plotted as the shaded region.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Temperature, MMW, and VMR as a function of pressure for the chemical equilibrium model of WASP-189 b. The P-T profile comes from F. Yan et al. (2020). The MMW and VMR values have been computed from the P-T profile using the FASTCHEM chemical equilibrium solver, assuming solar elemental abundances. For visual purposes we plot a selection of those most relevant to this work, although chemical abundances of additional atmospheric species were computed with FASTCHEM and included in the MMW. Left panel: P-T and MMW profiles. Middle panel: VMRs for the species shown in the legend below. The chemical profiles most relevant to this work (Fe, Si, Cr, Al) have been highlighted using thicker lines. Right panel: the emission contribution function for the fiducial spectral template. A spectral line core of neutral iron is highlighted, which forms at pressures of ∼0.1–1 mbar.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: S/N as a function of system velocity (vsys) and Keplerian velocity (Kp) when combining all out-of-eclipse phases for both nights in the barycentric rest frame. The literature values for vsys and Kp are indicated by the white dashed cross. The maximum S/N is marked by the small circle, and its value is annotated at the top of the plot. Top left: for the fiducial spectral template. Top right: for the neutral iron (Fe) spectral template using the chemical profile assuming equilibrium chemistry. Bottom: the fiducial spectral template without neutral iron.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Example of processing a spectral time series for the 141st spectral order and the second night. The color bar indicates photon counts, normalized to an appropriate value for each panel. (a) The raw spectral time series is normalized to its maximum value. (b) The spectral time series normalized to the continuum. (c) The same as in (b), but with the strongest telluric features masked and shown in gray. (d) After removal of the quasi-stationary components by SVD. (e) The same as in (d), but with the fiducial model injected at 10 times the nominal star-to-planet flux ratio. The strongest emission lines are visible as bright sloping lines, blueshifting due to the planet’s orbital acceleration.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Equilibrium chemistry spectral templates computed using PETITRADTRANS for the fiducial and single-species models over WINERED’s J band. These spectral templates do not include H− as a continuum opacity source. Spectra are offset by unity on the y-scale. Neutral iron has many strong lines and is prevalent in the fiducial model.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Signal-to-noise ratio per frame pair. Triangles pointing to the left indicate frame pairs observed during the first night, and crosses mark the second night. Blue and magenta colors indicate homogeneous pairs, whereas red and green colors indicates heterogeneous combinations. A clear pattern emerges, where the average S/N is higher for homogeneous pairs. We prefer a more stable S/N because our postprocessing algorithm can more easily remove quasi-stationary components.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: PSF-subtracted image of the inner region. The white lines represent the predicted location contours (1 and 2σ) of planet b by W. Thompson et al. (2025) during the time of the JWST observations, 2024 February 4. A blob within the expected position persists in PSF subtraction; however, given its proximity to the brightest speckle in the raw data and the noise structure in that location, we cannot rule out it being a residual from data reduction.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: Left: azimuthal average of the surface brightness as a function of offset from ϵ Eridani, using the images optimized for low-surface brightness extended emission recovery. Right: the surface brightness as a function of azimuth angle for between radial distances of 2﹩\mathop{.}\limits{^{\prime\prime} }﹩2 and 3﹩\mathop{.}\limits{^{\prime\prime} }﹩5. The East side of the inner disk region has an excess surface brightness of over 1σ standard deviation above the background. This is the forward facing side of the system, therefore larger scattered light emission would be expected here from an extended inner disk. The E–W asymmetry is also apparent in the image (Figure 8).