adsabs/AstroCLIMB huggingface dataset:
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Primary beam ellipticity as a function of frequency illustrates the activation of the TM11 mode toward the right of each respective band where the co-polarization beams are complementarily elongated. A larger fraction of the observable band is severely affected by this mode in the S band, beyond 3 GHz. There remains a narrow margin of variation in beam ellipticity among the different antennas in all bands, with somewhat more variability in the S band.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Maximum instrumental polarization and cross-polarization power as a function of frequency is shown at three different contour levels of Stokes I power of the main lobe. The envelopes at each power level show the spread over 16%–84% of antennas, representative of one standard deviation of variation among the different antennas.
Paper: A uvbyCaHβ CCD Analysis of the Open Cluster Standard, M67, and Its Relation to NGC 752
Authors: Bruce A. Twarog, Barbara J. Anthony-Twarog, Constantine P. Deliyannis
Figure caption: Correlation between distance in V above the ZAMS and the change in c 1 for stars at the turnoff in NGC 752. Blue circles define the relation for single stars. Red circles identify probable binaries.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Collimation errors due to indexer misalignment and slippage. Although the extreme slippage of m054 and m004 was corrected in 2021 July, m033 remains in significant error. Note that antenna m026 suffered a faulty receiver l.4058 installation that was swiftly removed. After servicing, this receiver was installed onto antenna m005 and thereafter m000 at later dates without recurring problems.
Paper: A uvbyCaHβ CCD Analysis of the Open Cluster Standard, M67, and Its Relation to NGC 752
Authors: Bruce A. Twarog, Barbara J. Anthony-Twarog, Constantine P. Deliyannis
Figure caption: CMD for stars in Figure 2. Symbols have the same meaning.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: The impact of environmental conditions, notably elevation and temperature, on the measured collimation errors in the L band. In the top panel only, results for the UHF and S bands (marked using U and S respectively) are included to show behavioral differences at high elevations among the bands in the horizontal direction due to asymmetrical gravitational loading of the indexer table. The applicable temperature color scale is shared in Figure 11.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Surface and collimation errors for all MeerKAT antennas measured at 60° elevation using L-band feeds as averaged over the time period from 2020 January to 2022 January. Contributions due to feed positioning and sub-reflector orientation as well as main reflector panel errors are included in these results, whereas antenna-pointing-error effects are removed. These are as for m028 in the second row of Figure 8.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Daily ambient temperature variability experienced at the MeerKAT site in the Karoo over the years from 2019 to 2022. An overnight cooldown of air temperature by 10°C is most common. Sunrise and sunset times are indicated using white dashed lines. A few cases of sensor failure can be seen, e.g., 2019 October 16–23 and 2021 July 22–23.
Paper: A uvbyCaHβ CCD Analysis of the Open Cluster Standard, M67, and Its Relation to NGC 752
Authors: Bruce A. Twarog, Barbara J. Anthony-Twarog, Constantine P. Deliyannis
Figure caption: The sem for each index and V as a function of V mag. The tick marks on the vertical scale for all panels define a change in the sem equal to 0.02 mag.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Effect of feed indexer table rotation error due to encoder mount slippage on the beams of antenna m054 with receiver l.4050 installed during the entire time frame. A 25° rotation of the fitted ellipse at the half-power point (dashed white lines) is measured on the Stokes I beam of 2021 June 25. The fault was corrected during 2021 July.
Paper: A uvbyCaHβ CCD Analysis of the Open Cluster Standard, M67, and Its Relation to NGC 752
Authors: Bruce A. Twarog, Barbara J. Anthony-Twarog, Constantine P. Deliyannis
Figure caption: Expanded turnoff region of the M67 CMD of Figure 7. Blue points are stars with anomalously blue colors.
Paper: A uvbyCaHβ CCD Analysis of the Open Cluster Standard, M67, and Its Relation to NGC 752
Authors: Bruce A. Twarog, Barbara J. Anthony-Twarog, Constantine P. Deliyannis
Figure caption: Cleaned CMD composed of probable members of M67, adjusted for (m − M) = 9.77 and E(b − y) = 0.021 and compared with isochrones of age 3.5 and 3.7 Gyr. The dashed green curve is the corrected cooler ZAMS of Figure 4 for NGC 752 superposed on the adopted isochrones. Green triangles represent additional photometric binaries.
Paper: A uvbyCaHβ CCD Analysis of the Open Cluster Standard, M67, and Its Relation to NGC 752
Authors: Bruce A. Twarog, Barbara J. Anthony-Twarog, Constantine P. Deliyannis
Figure caption: Same as Figure 2, but for M67. Blue and red symbols show stars classed as single and probable binary stars, respectively. Green symbols show stars classed via radial velocities as SB2 or triples. Blue asterisks show the location for single subgiants, while green open triangles indicate binary subgiants.
Paper: A uvbyCaHβ CCD Analysis of the Open Cluster Standard, M67, and Its Relation to NGC 752
Authors: Bruce A. Twarog, Barbara J. Anthony-Twarog, Constantine P. Deliyannis
Figure caption: Age derivation for NGC 752 from single stars using (m − M)0 derived solely from parallax, coupled with photometric reddening. Isochrones are metallicity-adjusted models of VR. The dashed green line represents an empirically derived correction to the isochrone lower main sequence.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Observed and modeled fluxes for hot Jupiters at secondary eclipse, in both the Spitzer 3.6 and 4.5 μm bands vs. planetary T eq and T irr. Fluxes from the no redistribution (NR) model are also plotted as a track, as well as the tracks for two blackbodies. The upper blackbody adopts zero albedo and no heat redistribution, whereas the lower blackbody adopts zero albedo and heat redistribution over the entire planet. The vertical dashed lines mark the 99% confidence regions for the quasi-discontinuous increase in flux (see text for discussion).
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Observed and modeled fluxes for hot Jupiters at secondary eclipse, in both the Spitzer 8 μm band and ground-based eclipses in the K band (2.3 μm) vs. planetary T eq and T irr. No redistribution (NR) model and blackbody tracks are overplotted as per Figure 2. The vertical dashed lines mark the 99% confidence regions for the quasi-discontinuous increase in flux (see text for discussion).
Paper: A uvbyCaHβ CCD Analysis of the Open Cluster Standard, M67, and Its Relation to NGC 752
Authors: Bruce A. Twarog, Barbara J. Anthony-Twarog, Constantine P. Deliyannis
Figure caption: Same as Figure 3, but for M67. Symbols have the same meaning as in Figure 5.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Examples of modeled emergent flux for planets with a range of temperatures, and in the wavelength region encompassing Spitzer’s 3.6 and 4.5 μm bandpasses (response curves at the bottom of the panels). The left panel shows models having solar metallicity, and the right panel is 30× solar metallicity for the same planets. The planets and their equilibrium temperatures are WASP-121b (T eq = 2358 K), XO-4b (1641 K), WASP-39b (1166 K), and HAT-P-12b (955 K). The vertical red markers at 4.5 μm call attention to carbon monoxide emission from a temperature inversion in WASP-121b.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Ratio of emergent flux to the flux from the no redistribution (NR) model vs. equilibrium and irradiation temperature. Each of the 437 points is a single Spitzer eclipse, except for a few planets (WASP-29, HAT-P-12, and HAT-P-15) where we averaged several eclipses due to low signal-to-noise ratio. Several outlying points lie above the range of this plot, but they have been included in the analysis. The fluxes exhibit an abrupt rise at an equilibrium temperature exceeding 1730 K, and the horizontal lines mark the inferred levels (ratios of 0.58 and 0.70). The amplitude of the rise corresponds to a brightness temperature increase of 210 ± 22 K, consistent among the different wavelength bands. The lower trace is the posterior distribution for the rise position, based on the analytic Bayesian methodology of Lee & Heghinian (1977). The horizontal scale of the posterior distribution for the solid line has been expanded graphically by a factor of 5, to make the shape more visible. For visual clarity, we do not plot error bars on the X-axis (temperature), but those uncertainties (median value ±19 K) were included when deriving the posterior distribution for the temperature of the flux rise.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Brightness temperature ratio (T  b  at 4.5 μm divided by T  b  at 3.6 μm) vs. equilibrium temperature. The tracks of points in slate blue and blue-violet colors are theoretical points from the models (solar metallicity, and 30× solar metallicity). The black line is a least-squares fit that considers error bars in both the X- and Y-coordinates (error bars in X are not plotted, to keep the figure clear). The slope of the fitted line differs significantly from zero (see text), and the model tracks come close to bracketing the observed points for equilibrium temperatures below ∼1200 K.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Brightness temperature difference (T  b  minus T eq) vs. equilibrium temperature. Each point represents the average of all eclipses for a given planet in a given wavelength band (see color legend). The location of the abrupt temperature rise is consistent with T eq = 1730 K (as in Figure 4), with amplitude ΔT  b  = 291 ± 49 K (see text). The red and blue lines are least-squares fits in the regimes hotter and cooler than the location of the abrupt temperature rise. The fits consider uncertainties in both the X- and Y-coordinates, but for visual clarity the (small) error bars on X are not plotted. The upward slopes of the lines are consistent with brightness temperature exceeding the equilibrium temperature by increasing amounts with increasing irradiance.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Color–flux diagram for hot Jupiters. The X-axis is the log of the flux ratio (4.5 μm flux divided by 3.6 μm flux) and the Y-axis the log of the 4.5 μm flux. The black line is a blackbody track, and the tracks for two collections of model planets are also included: solar metallicity models and 30× solar metallicity. The observed planets are color-coded by calculated equilibrium temperature.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Average eclipse depth per planet derived in this paper vs. literature values compiled by Baxter et al. (2020). The black lines are least-squares straight lines, and their slopes are within 2σ of unity, being 0.961 ± 0.020 and 1.008 ± 0.025 at 3.6 and 4.5 μm, respectively. The red mark on the 3.6 μm panel marks the outlying point for HD 189733b; see text in Section C of the Appendix for discussion.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: 3.6 and 4.5 μm points from Figure 4, binned over intervals of 100 K, with error bars based on the standard deviation (scatter) within each bin, divided by the square root of the number of points in that bin (standard error of the mean). The bin centers are nominally at multiples of 100 K in equilibrium temperature, but the points deviate slightly in X because we average both the X- and Y-values within each bin. We plot only the 3.6 and 4.5 μm points so as to maximize the clarity of the abrupt rise in flux. The vertical dashed lines are the 99% confidence limits that we infer for the temperature of the abrupt rise in flux. Note also that the data plotted here were not used directly in our analysis; this figure is only to make the flux rise optimally visible to the eye.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Ratio of the average eclipse depth per planet (ours divided by B20) vs. planet equilibrium temperature. We find no systematic variations at either wavelength as a function of equilibrium temperature. The red mark indicates the outlier Kepler-13b, discussed in Section C of the Appendix.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Histogram of Allan deviation slopes for the residuals (data minus fit) of 439 eclipses (3.6 and 4.5 μm both included). The blue curve is the best-fitting Gaussian that represents the distribution of slopes, and it peaks at −0.48, with a standard deviation of 0.047.
Paper: Emergent Spectral Fluxes of Hot Jupiters: An Abrupt Rise in Dayside Brightness Temperature Under Strong Irradiation
Authors: Drake Deming, Michael R. Line, Heather A. Knutson, Ian J. M. Crossfield, Eliza M.-R. Kempton, Thaddeus D. Komacek, Nicole L. Wallack, Guangwei Fu
Figure caption: Eclipses of planets not previously published and including WASP-29b, which was only recently published by Wong et al. (2022). In these plots, the data have been binned, and binning scales are adopted so that the data for each eclipse plot are spanned by 50 plotted points. The 50-point binning is only for uniformity of illustration; the actual binning used in fitting for the eclipse depths is different in all cases. The X-axis of the plots is orbital phase, but values are not listed since the central phases of the eclipses are not analyzed in this paper.
Paper: Detecting Exomoons from Radial Velocity Measurements of Self-luminous Planets: Application to Observations of HR 7672 B and Future Prospects
Authors: Jean-Baptiste Ruffio, Katelyn Horstman, Dimitri Mawet, Lee J. Rosenthal, Konstantin Batygin, Jason J. Wang, 劲飞 王, Maxwell Millar-Blanchaer, Ji Wang, 吉 王, Benjamin J. Fulton, Quinn M. Konopacky, Shubh Agrawal, Lea A. Hirsch, Andrew W. Howard, Sarah Blunt, Eric Nielsen, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich, Jerry W. Xuan
Figure caption: Future prospects for exomoon detections around the brown-dwarf companion HR 7672 B (left) and planet HR 8799 c (right). Simulated sensitivity for Keck/KPIC I, Keck/KPIC II, Keck/HISPEC, and TMT/MODHIS are shown in colored curves assuming six nights of observations over 25 days. The sensitivity demonstrated in this work from ∼1.5 nights of KPIC observations is labeled as KPIC I (Data). The mass ratios of the Galilean satellites are shown as black dots for comparison. Their predicted scaled-up mass ratios, q, accounting for the larger mass, M, of the brown dwarf compared to Jupiter are shown as gray crosses (﹩q\propto \sqrt{M};﹩ Batygin & Morbidelli 2020). The Roche limit is computed for both a rigid and a fluid satellite, shown as the inner and outer grayed regions, respectively.
Paper: Detecting Exomoons from Radial Velocity Measurements of Self-luminous Planets: Application to Observations of HR 7672 B and Future Prospects
Authors: Jean-Baptiste Ruffio, Katelyn Horstman, Dimitri Mawet, Lee J. Rosenthal, Konstantin Batygin, Jason J. Wang, 劲飞 王, Maxwell Millar-Blanchaer, Ji Wang, 吉 王, Benjamin J. Fulton, Quinn M. Konopacky, Shubh Agrawal, Lea A. Hirsch, Andrew W. Howard, Sarah Blunt, Eric Nielsen, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich, Jerry W. Xuan
Figure caption: RV precision and detectable mass ratio of MODHIS, similar to Figure 5 but as a function of planet mass, distance, and age of the system. Left: BT-Settl evolutionary models (Allard et al. 2012b) were used to infer the mass of the planet and distance to the system at an age of 3, 30, and 300 Myr. The minor contour lines cover an evenly spaced, 50-step log scale from 0 to 1 km s−1. RV sensitivity decreases the farther the system is away and the lower in mass the planet is. The large decrease in RV sensitivity when the companion mass is below ∼13 M Jup for young systems is due to the difference in cooling rates between brown dwarfs and planets over time. Right: the mass ratio detectable by MODHIS assuming a fixed semimajor axis for the moon equal to that of Callisto (≈26 R Jup). For each planetary mass and distance from panel (a), we create an RV time series assuming six nights of observations over 25 days, with error bars that represent the RV sensitivity calculated by PSIsim.
Paper: Detecting Exomoons from Radial Velocity Measurements of Self-luminous Planets: Application to Observations of HR 7672 B and Future Prospects
Authors: Jean-Baptiste Ruffio, Katelyn Horstman, Dimitri Mawet, Lee J. Rosenthal, Konstantin Batygin, Jason J. Wang, 劲飞 王, Maxwell Millar-Blanchaer, Ji Wang, 吉 王, Benjamin J. Fulton, Quinn M. Konopacky, Shubh Agrawal, Lea A. Hirsch, Andrew W. Howard, Sarah Blunt, Eric Nielsen, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich, Jerry W. Xuan
Figure caption: Exomoon detection limits around HR 7672 B with the Keck Planet Imager and Characterizer (KPIC) using the open-source Python module RVsearch (Rosenthal et al. 2021). Left: periodogram of the RV times series shown in Figure 2 expressed as a ΔBIC comparing a model with and a model without a planet. The empirical detection threshold is indicated in the legend. Right: exomoon completeness derived from injection and recovery tests. The periodogram and the completeness are shown for two cases: the single full night of observations on 2022 April 7 and all the available data including three additional epochs with 1–2 hr of data each. The variable conditions on 2022 April 7 led to HR 7672 B to not be detected during portions of the night, or in the RV precision to get significantly worse. By simulating RV time series, we estimate that the lost data only affected the final sensitivity by 20%.
Paper: Detecting Exomoons from Radial Velocity Measurements of Self-luminous Planets: Application to Observations of HR 7672 B and Future Prospects
Authors: Jean-Baptiste Ruffio, Katelyn Horstman, Dimitri Mawet, Lee J. Rosenthal, Konstantin Batygin, Jason J. Wang, 劲飞 王, Maxwell Millar-Blanchaer, Ji Wang, 吉 王, Benjamin J. Fulton, Quinn M. Konopacky, Shubh Agrawal, Lea A. Hirsch, Andrew W. Howard, Sarah Blunt, Eric Nielsen, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich, Jerry W. Xuan
Figure caption: RV precision of MODHIS. Left: the RV sensitivity of MODHIS for model planets around a HR 8799–like host star using BT-Settl models (Allard et al. 2012a). The RV sensitivity was predicted using PSIsim for a single, 2 hr exposure. Both the contour curves and color map indicate the RV sensitivity for a specified effective temperature and apparent magnitude of the model planet. The RV sensitivity relies more on the brightness of the planet than its effective temperature. However, the RV sensitivity decreases for planets with temperatures between 1500 and 1700 K due to the L/T transition. Right: the RV semi-amplitude for different planet masses and mass ratios. Note, increasing the exposure time will increase the RV sensitivity.