adsabs/AstroCLIMB huggingface dataset:
Paper: HST UV Spectroscopy of the Planet-hosting T Tauri Star PDS 70
Authors: Stephen L. Skinner, Marc Audard
Figure caption: PDS 70 G140L and G230L continuum flux densities measured in narrow wavelength intervals and dereddened using A  V  = 0.05 and the extinction law of Whittet et al. (2004) Flux densities are in units of 10−16 erg cm−2 s−1 Å−1 . The sloping blue line at far right is a power-law fit to four dereddened photospheric continuum measurements (Table 3) F  λ,dered =−101.5 + 0.1947λ +0.7978 extrapolated to zero flux density at λ = 2545 Å . The red dashed line at left shows the mean FUV MAMA background level (no dereddening) at F  λ,bgd = 5.42 × 10–17 erg cm−2 s−1 Å−1 . The curved line is a fit of 15 continuum data points (1282–2561 Å ) using an exponential model with a constant offset of the form F  λ,dered = C + Aexp[(λ − λ 0)/EW. Best-fit values are C = 0.5836, A = 0.2908, EW = 230.7, λ 0 = 1926. The data and model become indistinguishable from background at λ < 1600 Å .
Paper: HST UV Spectroscopy of the Planet-hosting T Tauri Star PDS 70
Authors: Stephen L. Skinner, Marc Audard
Figure caption: PDS 70 G140L gross (=source + background), net (=source − background), and background count rates from the combined exposures in a narrow wavelength interval where no significant line emission is expected. The background rate is based on the average of two background spectra extracted at offsets of ±300 pixels (±7.″5) from the stellar trace. Source and background rates were measured in spectra extracted with a width of 11 pixels in the cross-dispersion (spatial) direction.
Paper: HST UV Spectroscopy of the Planet-hosting T Tauri Star PDS 70
Authors: Stephen L. Skinner, Marc Audard
Figure caption: STIS/MAMA G140L spectra of PDS 70 and the K7e-type wTTS HBC 427 (=V397 Aur). The flux density of HBC 427 has been scaled up by a factor of 1.748 to correct for its greater distance (148.6 pc) than PDS 70 (112.39 pc). Error bars are not shown to facilitate comparison. The HBC 427 G140L archive spectrum (O8NS07020) is from a 1425 s observation on 2004 January 20 using the 52″ × 0.″2 slit. Note the lack of H2 lines in the HBC 427 spectrum.
Paper: HST UV Spectroscopy of the Planet-hosting T Tauri Star PDS 70
Authors: Stephen L. Skinner, Marc Audard
Figure caption: STIS/MAMA G140L spectrum of PDS 70 from combined exposures showing five prominent fluorescent H2 lines. Tick marks show lab wavelengths of the H2 transitions (Table 4). Weak neutral sulfur lines are marked at 1474 and 1483 Å.
Paper: HST UV Spectroscopy of the Planet-hosting T Tauri Star PDS 70
Authors: Stephen L. Skinner, Marc Audard
Figure caption: Raw STIS CCD acquisition image of PDS 70 taken through the F28X50LP filter showing a second faint source (Gaia EDR3 source_id 6110141563309613184) located ≈2.″5 northeast of PDS 70.
Paper: HST UV Spectroscopy of the Planet-hosting T Tauri Star PDS 70
Authors: Stephen L. Skinner, Marc Audard
Figure caption: STIS/MAMA G140L spectra of PDS 70 for the three exposures showing the C IV doublet (λ lab = 1548.19, 1550.78 Å). Solid black: exposure 1; dashed blue: exposure 2; dotted red: exposure 3. Error bars are shown only for the first exposure.
Paper: HST UV Spectroscopy of the Planet-hosting T Tauri Star PDS 70
Authors: Stephen L. Skinner, Marc Audard
Figure caption: STIS/MAMA G140L and G230L spectra of PDS 70 from the combined exposures with prominent emission lines identified. The O I line in G140L is geocoronal.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: The model ETVs (lines) and measurements (points) for primary (red) and secondary (blue) eclipses. The longer-term sinusoidal part of the red and blue curves represents driven apsidal motion of the 3.3 day binary by star B in its 51 day orbit. The apsidal motion period is relatively short at only ≃4 yr. The more rapid sinusoids at a ∼51 day period represent the largely dynamical delays that result from the orbit of star B around the A binary. These two effects alone constitute independent and dramatic proof that star B orbits the A binary. The last six points denoted with orange and cyan colors were obtained only after the completion of the photodynamical modeling process and were therefore not used for the fitting. It can be seen, however, that they align nicely with the model as predicted.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: Left panel: orbital motions of star C (green), star B (red), center of mass of binary A (Acm;  blue), and center of mass of binary A-B (ABcm) in black, all drawn according to our final model (see Table 4). The observers are viewing the system from Y = −∞, but the reader is looking down on the orbits from Z = +∞. Right panel: schematic showing how the velocities of the stars conspire to slow the relative motion of star C and Acm on the sky during TESS sector 14, thereby making the third-body eclipses last for ∼12 days. While the motion of ABcm is opposite to that of C (thereby causing a high relative speed), the orbital motion of Acm within the A–B binary is opposite that of ABcm only at this particular phase of the A–B binary and is therefore in the same direction as that of star C, thereby slowing the relative motion. Note that the velocities are scaled approximately correctly, while the vertical separation of the stars is not at all to scale.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: A section of the TESS sector 40 light curve. The pale blue points are the original (but detrended), 600 s cadenced Fitsh FFI photometry points, while the dark blue around the regular eclipses denote the 1800 s binned points used for the photodynamical MCMC modeling. Residuals are shown in the bottom panel.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: A secondary eclipse of the innermost binary observed by H. Kučáková on the night of 2022 May 9/10 with a Cousins R C filter on the 0.65 m Mayer telescope of the Ondřejov observatory, CZ. Here, the smaller, lighter blue dots represent the original 60 s exposure time observations, while the larger, darker blue circles stand for their 600 s bins used for the modeling. Residuals are shown in the bottom panel.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: The TESS sector 14 data points (blue) and the model (red) curve during the third-body event. Note the predicted eclipse in the data gap. Residuals are shown in the bottom panel.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: The fit of our model (see Section 7) to the TRES RVs shows two orbits: one at 51.18 days and the other 2099 days. These are taken to be the orbits of the inner triple, AB, and the quadruple, ABC, respectively. Our model RVs are shown for star B in red and star C in blue.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: Model light curve of TIC 114936199 for the 21st century.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: Schematic of TIC 114936199, with the periods of each orbit.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: Left: the evolution of the PF using NICER data. The vertical dashed green line shows the luminosity where the PF evolution changes from increasing to decreasing. The vertical dashed black line presents the critical luminosity suggested by Figure 2, where the increasing slope of the PF becomes flatter. Right: the energy dependence of PF from 1 to above 130 keV using Insight-HXMT data. All the error bars are given at the 68% confidence level. Note that the high PF in 27–50 keV is most likely due to the prominent peak around 30–40 keV in the Insight-HXMT background model (see Figures 5 and 10 in Liao et al. 2020), which causes an oversubtraction of the background when calculating the PF.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: Pulse profiles of RX J0209.6−7427 from Insight-HXMT observations. The profiles are normalized to the mean value in each energy band, and two rotational periods are shown for clarity. Vertical 1σ error bars are derived from the counting statistics by assuming Poisson fluctuations. The number of bins in each energy band was simply determined based on the photon statistics. Vertical dotted lines indicate the ON pulse and OFF pulse definitions for both the main and minor peaks. (A) (0.32–0.62): ON pulse of the minor peak (shaded area); (B) (0.62–1.26): ON pulse of the main peak; (C) (0.26–0.32): OFF pulse of the main and minor peaks. We cannot exclude the possibility of a phase-dependent absorption spectral feature (possibly a CRSF for ∼1013 G surface magnetic field of the NS) at energy around 100 keV, which may cause the dip at phase around 0.55 in the pulse profile of 80–130 keV band.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The 5-observation combined spectrum of the main peak of RX J0209.6−7427 observed with the Insight-HXMT during the 2019 outburst. The lower panel of each spectrum shows the residuals to the best-fitting model. Top: fitted using the OFF spectrum as background in the energy band of 1–150 keV, the best-fit model is Tbabs∗(cutoffpl+bbodyrad). Bottom: fitted using the Insight-HXMT background model in the energy band of 1–50 keV. The best-fit model is Tbabs∗(cutoffpl+bbodyrad+bbodyrad+Gaussian). Above 50 keV, the Insight-HXMT background uncertainty (∼1%) is comparable to the flux of the source emission, so it is inappropriate to include data above 50 keV. The absorption-like feature at around 40 keV in the residuals is due to the structure in the background model around this energy.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The 5-observation combined phase-averaged spectrum of RX J0209.6-7427 observed with the Insight-HXMT during the 2019 outburst in the energy band of 1–50 keV fitted with the Tbabs∗(cutoffpl+bbodyrad+Gaussian) model using the Insight-HXMT background model. Above 50 keV, the Insight-HXMT background uncertainty (∼1%) is comparable to the flux of the source emission, so it is inappropriate to include data above 50 keV. The absorption-like feature at around 40 keV in the residuals is due to the structure in the background model around this energy. The lower panel shows the residuals to the best-fitting model.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: (a), (b), (c), (d): examples of cross correlation of different HE pulse profiles with the LE 1–10 keV profile. In each example, the upper panel shows the cross correlation vs. phase lag for a given HE profile with the LE 1–10 keV profile. The lower panel shows the cross-correlation distribution from 106 Monte Carlo simulations of two noncorrelated profiles.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The 5-observation combined spectrum of the minor peak of RX J0209.6−7427 observed with the Insight-HXMT during the 2019 outburst in the energy band of 1–30 keV. The lower panel of each spectrum shows the residuals to the best-fitting model. Top: fitted using the OFF spectrum as background, the best-fit model is Tbabs∗cutoffpl. Bottom: fitted using the Insight-HXMT background model, the best-fit model is Tbabs∗(cutoffpl+bbodyrad+Gaussian).