adsabs/AstroCLIMB huggingface dataset:
Paper: Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N
Authors: Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson
Figure caption: Various HARPS-N stellar activity indicators versus HD 79211's radial velocities after the stellar binary trend has been subtracted. The r-values are Pearson correlation coefficients. All of these parameters are weakly correlated, with r-values less than 0.3.
Paper: Perihelion Activity of (3200) Phaethon is Not Dusty: Evidence from STEREO/COR2 Observations
Authors: Man-To Hui, 文韜 許
Figure caption: Phaethon in COR2 images around different perihelion returns. The images are median stacks from individual images taken by the same cameras in the same apparitions with alignment on the ephemeris motion of Phaethon (marked by a green circle in each panel). We are unable to confidently detect Phaethon in the observations taken at large phase angles (COR2-B in the apparitions of 2009 and 2013, COR2-A in 2019 and 2022). J2000 equatorial north is up and east is left. A scale bar of 5′ in length applicable to all of the panels is shown in the lower-left corner.
Paper: Perihelion Activity of (3200) Phaethon is Not Dusty: Evidence from STEREO/COR2 Observations
Authors: Man-To Hui, 文韜 許
Figure caption: Example of fitting the photometric parameters for a COR2-B image from 2012 May 3. Field stars used and rejected in the Levenberg–Marquardt optimization are plotted as olive filled and open circles, respectively. The best-fit function is shown as the red dashed line. In the lower-left corner, we present the number of used stars and the image zero-point (abbreviated as “ZP” therein).
Paper: Perihelion Activity of (3200) Phaethon is Not Dusty: Evidence from STEREO/COR2 Observations
Authors: Man-To Hui, 文韜 許
Figure caption: Zero-points of COR2 images in their respective bandpasses vs. time. Data points of COR2-A and COR2-B are plotted in red and blue, respectively. The dotted lines are weighted mean zero-point values of the two cameras. There is tentative evidence that the zero-points have been changing over time; however, the uncertainties are too large for further interpretation.
Paper: Perihelion Activity of (3200) Phaethon is Not Dusty: Evidence from STEREO/COR2 Observations
Authors: Man-To Hui, 文韜 許
Figure caption: Transits of Phaethon in the annular FOVs (bounded by two concentric circles) of (a) COR2-A and (b) and COR2-B cameras. Trajectories from different apparitions are distinguished by different colors. The positions are plotted every two hours, with the first positions inside the FOVs indicated by symbol “+” in the same colors. Corresponding epochs in UTC are given in the legends. The bold plus sign in black at the center of either panel represents the center of the Sun.
Paper: Perihelion Activity of (3200) Phaethon is Not Dusty: Evidence from STEREO/COR2 Observations
Authors: Man-To Hui, 文韜 許
Figure caption: Reduced magnitude of Phaethon vs. phase angle. COR2-A and COR2-B observations are color coded in red and blue, respectively. Detections are shown as filled circles, whereas nondetections are shown as open circles. For comparison, we plot two models corresponding to light scattering of Phaethon dominated by its nucleus (dashed line, with the neighboring shaded area representing the ±1σ uncertainty region) and a coma consisting of μm-sized dust grains (black dotted line, with the ±1σ uncertainty region marked by two bracketing gray dotted lines). It is obvious that the obtained reduced magnitude measurements of Phaethon in the COR2 images are in line with the nucleus model but deviate considerably from the dusty coma model.
Paper: Perihelion Activity of (3200) Phaethon is Not Dusty: Evidence from STEREO/COR2 Observations
Authors: Man-To Hui, 文韜 許
Figure caption: Modeled flux (in arbitrary units) of Phaethon due to Fe I emissions transmittable in the HI-1 cameras (wavelengths λ ≈ 400 nm). In the top panel, the production rate of iron is assumed to be ﹩\sim {r}_{{\rm{H}}}^{-5}﹩, whereas ﹩\sim {r}_{{\rm{H}}}^{-10}﹩ is assumed in the bottom panel. Different colors of the curves correspond to the peak of the iron production rate delayed by different amounts of time (labeled in the legend) from perihelion.
Paper: Perihelion Activity of (3200) Phaethon is Not Dusty: Evidence from STEREO/COR2 Observations
Authors: Man-To Hui, 文韜 許
Figure caption: Fluorescence efficiencies (g-factors, in the unit of photons per atom per second) of Fe I (upper panel) and Na D (lower panel) emissions in the current orbit of Phaethon around perihelion. The dips at perihelion are due to the overlaps with the solar Fraunhofer absorption lines.
Paper: Perihelion Activity of (3200) Phaethon is Not Dusty: Evidence from STEREO/COR2 Observations
Authors: Man-To Hui, 文韜 許
Figure caption: Same as Figure 7, but for Na D-line emissions.
Paper: Detecting Isolated Stellar-mass Black Holes with the Roman Telescope
Authors: Sedighe Sajadian, Kailash C. Sahu
Figure caption: Two examples of simulated magnification curves. The left panels show the magnification curves with (dashed curves) and without (dotted curves) the parallax effect. The right panels show the corresponding astrometric motions of the source stars (blue curves), lens objects (magenta curves), and their relative motions (dark red curves) projected on the sky plane. The synthetic data are taken with the Roman telescope. The observable parameters for each panel are mentioned at the top of the light curves and astrometric plots.
Paper: Detecting Isolated Stellar-mass Black Holes with the Roman Telescope
Authors: Sedighe Sajadian, Kailash C. Sahu
Figure caption: The normalized (fractional) distributions of t E, m base, t 0, and u 0 for all the microlensing events detected by Roman, depicted in green. Also, the normalized distributions of the events for which the physical parameters of the lenses will be measurable with ≤5% relative errors (after considering the extra observations during the ∼2.3 yr time gap) are shown as the black stepped curves. The average values of these parameters are calculated from the related distributions that are mentioned in the legends.
Paper: Detecting Isolated Stellar-mass Black Holes with the Roman Telescope
Authors: Sedighe Sajadian, Kailash C. Sahu
Figure caption: The same as Figure 1, but considering extra observations—1 hr observations of the Galactic bulge, every 10 days, when the bulge is observable during the ∼2.3 yr time gap—with the Roman telescope. These extra data points are depicted in green.
Paper: Detecting Isolated Stellar-mass Black Holes with the Roman Telescope
Authors: Sedighe Sajadian, Kailash C. Sahu
Figure caption: The fractional distributions of the relative errors in the normalized parallax amplitude, the lens mass, the lens distance, and the lens proper motion for a large sample of microlensing events due to ISMBHs detectable by the Roman telescope, with (green distributions) and without (black stepped distributions) considering sparse observations when the Galactic bulge is observable during the large time gap. The vertical (solid, dashed, and dotted) lines show the thresholds of the relative errors of 10%, 5%, and 1%, respectively. The samples for both distributions have the same entrances.
Paper: Detecting Isolated Stellar-mass Black Holes with the Roman Telescope
Authors: Sedighe Sajadian, Kailash C. Sahu
Figure caption: The dependence of the average relative errors in the lens mass (solid green lines), the lens distance (dashed blue lines), the proper motion (dotted–dashed magenta lines), and the normalized parallax amplitude (dotted red lines) vs. the lens mass, the ratio of the lens distance to the source distance from the observer (x ls), the source distance, and the source apparent magnitude at the baseline.
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Top: quartic fit to the spectrum of Sirius; the solid line is the spectrum and the dotted one the fit. The short gap in the spectrum is where a spectral feature has been masked. Bottom: residuals in the fit, shown as fit—spectrum. The quartic fit is shown as a solid line and a power-law fit as a dashed one.
Paper: Detecting Isolated Stellar-mass Black Holes with the Roman Telescope
Authors: Sedighe Sajadian, Kailash C. Sahu
Figure caption: The Galactic plane and the two coordinate systems that are needed to project stellar velocities on the sky plane.
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Equatorial rotation velocities for early A-stars from Abt & Morrell (1995), along with the equatorial rotation velocity value for Vega from Aufdenberg et al. (2006).
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Dependence of V − K  S  on vsini for A0V stars, using photometry from 2MASS and Hipparcos. The blue circles are “normal” stars while the red triangles are Am(0)V and Ap(0)V stars; the line is a fit to the normal stars. The orange diamonds are for Vega (small vsini) and 109 Vir; because they are bright and saturated in recent photometry, the photometry is from Leggett et al. (1986), Rieke et al. (2008), and Mermilliod (1991). The vsini for the latter star (Royer et al. 2007) is virtually identical to the equatorial velocity for Vega (Aufdenberg et al. 2006). The scatter in V − K  S  substantially exceeds that expected from the photometric errors (≤0.03 mag). The underlying cause for the scatter is illustrated by the comparison of the Am and Ap stars with Vega, all with similar values of vsini but significantly different in V − K  S .
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption:  V − K  S  vs. T eff for dwarf stars with temperatures similar to that of the Sun. The temperatures have been taken from the line depth ratio (LDR) results of Kovtyukh et al. (2003), the K  S  photometry from 2MASS or heritage photometry transformed to 2MASS, and the V photometry from Hipparcos, transformed from H  p  to V, as in Harmanec (1998). The central red point is at the solar temperature (5772 K) with error bars of ±0.03 in V − K  S  and ±50 K in T eff. The line is the linear fit given in Equation (6).
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Spectral shapes compared to that of a 5750 K star similar to the Sun, for two alternative stellar temperatures with the reddening adjusted to create as close a match as possible over the entire 0.4–30 μm range (spectra from the BOSZ database, Bohlin et al. 2017, with log g = 4.5 and the other parameters set to the solar values). The ratios have been adjusted to an average of 1 for easy comparison. The ratios have been running median-averaged to smooth over absorption lines with the expectation that any use of a star for absolute calibration would interpolate over them.
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Spectral shape comparisons for A-stars of various temperatures, based on models from the BOSZ database (Bohlin et al. 2017), log g = 4.0, the other parameters set at the solar values. As in Figure 10, the reddening has been adjusted to create as close a match as possible over the entire 0.4–30 μm range. The ratios have been adjusted to an average of 1 for easy comparison, and the ratios have been running median-averaged to smooth over absorption lines. The results apply to ideal A-stars with no temperature gradients (i.e., slow rotators) and no hot dust excesses.
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Template spectrum for β Gem and measurements relative to Sirius. The spectrum of Sirius is from CALSPEC (Bohlin et al. 2020). Four templates are shown: (1) from Cohen et al. (1995); (2) from Engelke et al. (2006); (3) an updated version by Engelke; and (4) as derived in this paper combining the BOSZ model (λ < 6.5 μm) and the spectrum of HR 6348 (λ > 6.5 μm). The blue round points are photometry relative to Sirius as described in the text. The red diamond points are measurements obtained with MSX (Price 2004), also shown relative to Sirius.
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Adopted infrared spectrum of the Sun. As discussed in the text, the spectrum was constructed from a series of solar spectral observations and models. It agrees perfectly (within 1% with the photometry shown in the figure, extending from the H band (1.6 μm) through 15 μm (it is also in agreement with photometry at V to within 1%).
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Correction to pure Rayleigh–Jeans behavior of IRAC Band 1 to obtain accurate stellar surface flux estimates. Over this temperature range, the total amplitude is only ∼2%.
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: BOSZ spectra (normalized by 1/T eff plus correction term illustrated in Figure 7). The dashed lines are for T eff every 250 K from 4750–6750 K, the dotted lines for 7000–8250 K, and the solid lines for 8500–10,000 K. The point with error bars shows the FWHM of IRAC Band 1, and a ±1% vertical range.
Paper: Absolute Calibration. III. Improved Absolute Calibration for the Visible through the Mid-infrared
Authors: G. H. Rieke, Charles Engelke, Kate Su, Luca Casagrande
Figure caption: Ratio of stellar diameters determined by the IRFM to the limb-darkened diameters measured interferometrically, as a function of T eff.
Paper: Relation between Long-term Activity and Luminosity of the Pre- and Post-novae CT Ser and V446 Her
Authors: Vojtěch Šimon
Figure caption: (a) Long-term (both pre-nova and post-nova) activity of V446 Her. Data from several databases were merged: DASCH (Grindlay et al. 2012; closed circles for detections, short horizontal lines for upper limits), photographic plates of Cragg (1960; empty squares), and Stienon (1971; closed diamonds), RoboScope CCD data (Honeycutt et al. 2011; empty diamonds). The short horizontal lines represent the upper limits of brightness. The error bars of the data points are marked. (b) Light curves of the well-observed outbursts in post-nova V446 Her (CCD data after JD 2,448,000). The error bars would usually be comparable to the size of the symbols. The individual events were connected by the line to guide the eye. The individual events were shifted along the time axis to match the decaying branch of the template. The shifts (in days) of times of crossing 16.5 mags on the decaying branch of each well-covered outburst are listed. The value of the outburst decay rate τ D was measured for the steep part starting at the brightness of 15.5 mags, in some cases of 16.1 mags. See Section 4 for details.
Paper: Relation between Long-term Activity and Luminosity of the Pre- and Post-novae CT Ser and V446 Her
Authors: Vojtěch Šimon
Figure caption: Histograms of M opt of CT Ser and V446 Her in various activity states. The solid bar in panel (b) marks the minimum absolute magnitude of V446 Her in its pre-nova phase (Cragg 1960). The vertical long-dash line represents M opt of maxima’s peaks of DN outbursts analyzed by Patterson (2011), appropriate to P orb of CT Ser and V446 Her. The short-dashed lines mark its error bars. The vertical lines in the upper-right corner of each plot represent the deviations of M opt in the B-band in the upper or lower limit of d from its best value (the longest central vertical line) given in Bailer-Jones et al. (2021). The values of A  V  and A  B  from Sections 3 and 4 remained unchanged for a given CV. See Sections 3 and 4 for details.
Paper: Relation between Long-term Activity and Luminosity of the Pre- and Post-novae CT Ser and V446 Her
Authors: Vojtěch Šimon
Figure caption: (a) Long-term activity (from pre-nova to post-nova) of CT Ser. Data from several databases were merged: DASCH (Grindlay et al. 2012; circles for detections, short horizontal lines for upper limits), and CRTS (Drake et al. 2009; empty diamonds). The error bars of the data points are marked. The oblong near JD 2,442,000 refers to the Palomar Green Survey (Green et al. 1986). The oblong near JD 2,449,000 represents the flux level of the spectra (Ringwald et al. 1996). (b) Transition to a plateau of the CN outburst or a start of the post-nova in CT Ser (the DASCH data, short horizontal lines are the upper limits). (c) Random deviations from the mean brightness of the post-nova CT Ser (the CRTS data). The points were connected by a line in the densely covered parts of the light curve to guide the eye. (d) Histogram of the brightness from panel (c).
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: The maximum difference in directivity power between the Stokes I beams for all antennas and that of the array average is shown in the top row of panels for the respective bands as evaluated over the half-power region of the beam after accounting for antenna-pointing errors. These error-beam performance profiles show that larger variations of the beam shape among antennas exist in the lower half of the S band compared to that of the other bands. In the second row, the maximum instrumental polarization induced over the half-power region of the beam is shown (not instrumental polarization error as in Table 3). While the instrumental polarization seems improved in the S band at more frequencies than the other bands, some more spikes of poorer performance occur at intermittent frequencies. The last row shows the maximum power of either cross-polarization beam that occurs over the half-power region of the Stokes I beam relative to the peak Stokes I power. A few outlier cases are illustrated in color. The degraded Stokes I error-beam performance of m033 in the top row is mostly affected by an exceptionally large feed indexer error that manifests as a horizontal (cross-elevation) feed-position error causing beam shear and coma lobes. It is interesting to note that, despite m033's poor Stokes I performance, its polarization performance is not as bad because the cross-polarization pattern is more (but not only) sensitive to the characteristics of the feed package installed rather than reflector collimation effects.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Main reflector panel surface errors for antenna m028 are computed at 60° elevation in each of the MeerKAT bands for the H-polarization. The aperture plane phase maps, hence path-length errors, are expressed as surface deviation errors relative to a parabolic dish surface. The top row shows that frequency-dependent features superimposed onto the aperture plane phase are more substantial at lower frequencies and are almost absent in the Ku band. In the second row, for the UHF, L, and S bands, the frequency-invariant phase component over the respective band is shown, revealing phase effects due to collimation errors. In the third row, feed-positioning phase errors are removed and in the final row sub-reflector orientation errors are also removed. In the single-frequency Ku-band result, the small contribution from the feed-phase front manifests as a green counterclockwise tilted bowtie pattern in the center of its map, is not removed here. This feature could be removed using either array average information, which is not available in the Ku band, or less accurately, by using EM simulation results. Note that different feed-position errors exist for each band due to their unique mounting errors on the feed indexer. Antenna m028 is chosen in this example because its collimation has remained stable over time and this is the only antenna for which recent Ku-band measurements are available. The Ku measurement is dated 2021 August 17, at an elevation of 52°.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Frequency-dependent pointing of MeerKAT primary beams in the horizontal direction reveals the activation of the asymmetrical TE21 waveguide mode as deviations to the left and right. Results for a few outlier receivers are indicated using color to emphasize that, even though a range of variation is indicated for many different receivers in gray scale, the characteristics of individual receivers are unique and do not change over time. Antenna pointing in the horizontal direction is zeroed at 900, 1420, and 2625 MHz in the UHF , L and S bands, respectively, using the vertical co-polarization profile. Note that the overlapping 856–1088 MHz range of the L-band receiver may be preferred in polarization studies over that of the UHF receiver due to the increasing effect of higher order waveguide modes toward the upper part of each band.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Frequency-dependent pointing of MeerKAT primary beams in the vertical direction reveals the activation of the asymmetrical TE21 waveguide mode as deviations up and down. Antenna pointing in the vertical direction is zeroed at 900, 1420, and 2625 MHz in the UHF , L, and S bands, respectively, using the horizontal co-polarization profile. An inset axis highlights the resonant activation of a ghost mode (of TE21) that propagates and differs in character slightly per receiver.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: The half-power beamwidth measurements show that the MeerKAT Stokes I primary beams are consistently narrower in the horizontal direction across all bands. Very narrow margins of variation in beam widths are noted among all antennas in the UHF and L bands. Dramatic beam shape elongation features occur as a result of the activation of the TM11 waveguide mode toward the upper end of each band due to respective OMT designs, more prominently in the S band.
Paper: MeerKAT Holography Measurements in the UHF, L, and S Bands
Authors: Mattieu S. de Villiers
Figure caption: Path-length errors modeled by means of ray tracing are illustrated as contours over the extended aperture (17 m across). The contours are spaced at 0.1 mm per mm (path-length error per position error) for the first four panels, and 0.1 mm per quarter degree (path-length error per rotational alignment error) for the last two panels. Negative values are indicated using dashed lines.