adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: The shaded regions in the figure above represent the predicted beat frequencies between the WD spin frequency and diamagnetic blobs orbiting at the circularization radius with a Keplerian orbit. Because the masses of the stellar components are unknown, we parameterized the predicted frequency against a range of plausible stellar mass ratios. The two limiting cases, blobs interacting with one pole or interacting with both poles equally, defines the range of plausible frequencies at each mass ratio. The dark green region represents the upper and lower bound of V2400 Oph’s QPOs (2–9 cycles d−1) produced through two-pole interaction while the light green region defines the range for one-pole interaction.
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: Trailed Lomb–Scargle periodogram of the K2 light curve of V2400 Oph, binned at 1.25 days with 0.25 day step increments. The dominant signals are located within the QPO range, and the amplitudes of the (ω − Ω), (ω), and 2(ω − Ω) signals all vary sporadically throughout the observation (T 0 ≈ 2823.33559 BKJD).
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: The top and bottom panels show ∼14 hr segments of the K2 V2400 Oph light curve when the beat signal is at ∼ 100% and ∼ 50% its maximum amplitude, respectively. In both segments, a low-frequency oscillation at ∼5 cycles d−1 is clearly identifiable and accounts for the large flux variations. The K2 V2400 Oph light curve demonstrates more aperiodic fluctuations and chaotic nature than normally observed in CVs. (T 0 ≈ 2823.33559 BKJD).
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: A binned, Lomb–Scargle periodogram of the K2 V2400 Oph data set. The break in slope at ∼102 cycles d−1 is common among disk-fed systems (Scaringi 2014).
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: Correlations between relative brightness and signal amplitudes of both V2400 Oph and FO Aqr K2 observations. Each data point corresponds to a 1.5 days observation window. FO Aqr shows some correlation between each signal and the relative brightness of the system. The V2400 Oph signals appear to be uncorrelated with the system’s brightness.
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: Scatter plots of the K2 data demonstrating the uncorrelated beat signal amplitude with other signals in the system. Each point corresponds with a ∼5 hr observation window.
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: Relative phase change for spin and beat signals over the duration V2400 Oph and FO Aqr K2 observations. Each data point corresponds to a 1.5 days observation window. The FO Aqr spin signal phase is by far the most stable showing minimal variation compared to the other three signals. The FO Aqr and V2400 Oph beat signals show similar levels of phase variability over their respective observations.
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: The dominant signal and signal amplitudes as a function of observation window size for the K2 light curve. The probability of observing a given signal with the highest relative amplitude is significantly influenced by the observation length.
Paper: Rotation Period Detection for Earth-like Exoplanets
Authors: Jiazheng Li, Jonathan H. Jiang, Huanzhou Yang, Dorian S. Abbot, Renyu Hu, Thaddeus D. Komacek, Stuart J. Bartlett, Yuk L. Yung
Figure caption: The minimum length of observation needed to detect the rotation period as functions of the wavelength and orbital geometry. We combine 1 and 2 day period data here (see Section 4.2) and use a 99% confidence threshold. The time resolution is 12 data points per period. The observational error is 5%. (a) Azimuthal-rotated edge-on orbital geometries (see Figure 1). (b) Polar-rotated orbital geometries. The color white indicates that the rotation period is not detectable.
Paper: Rotation Period Detection for Earth-like Exoplanets
Authors: Jiazheng Li, Jonathan H. Jiang, Huanzhou Yang, Dorian S. Abbot, Renyu Hu, Thaddeus D. Komacek, Stuart J. Bartlett, Yuk L. Yung
Figure caption: How we derive the rotation period from a time series. (a) A simulated time series of reflected starlight for the 1 day rotation period experiment. (b) The detrended time series. (c) Fourier transform of the detrended time series. (d) Signal-to-noise ratio as a function of period. The red line indicates the signal-to-noise threshold for 99% confidence.
Paper: Rotation Period Detection for Earth-like Exoplanets
Authors: Jiazheng Li, Jonathan H. Jiang, Huanzhou Yang, Dorian S. Abbot, Renyu Hu, Thaddeus D. Komacek, Stuart J. Bartlett, Yuk L. Yung
Figure caption: Two divergent sets of orbital geometries used in this study. On the top of each panel, the small diagram shows how we rotate the orbit to obtain different orbital geometries. The diagrams below show the correspondence between the angles and the orbital geometries. (a) The exoplanet is in an azimuthal-rotated edge-on orbit. (b) The exoplanet is in a polar-rotated orbit. The markers next to each diagram represent the orientation of the sunlit disk in the view of the observer.
Paper: Rotation Period Detection for Earth-like Exoplanets
Authors: Jiazheng Li, Jonathan H. Jiang, Huanzhou Yang, Dorian S. Abbot, Renyu Hu, Thaddeus D. Komacek, Stuart J. Bartlett, Yuk L. Yung
Figure caption: An example of the minimum length of observation needed to detect the rotation period as a function of wavelength. We combine 1 and 2 day period data here (see Section 4.2) and use a 99% confidence threshold. The orbital geometry is 180° of the azimuthal-rotated edge-on orbit, the time resolution 12 data points per period, and the observational error is 5%.
Paper: Rotation Period Detection for Earth-like Exoplanets
Authors: Jiazheng Li, Jonathan H. Jiang, Huanzhou Yang, Dorian S. Abbot, Renyu Hu, Thaddeus D. Komacek, Stuart J. Bartlett, Yuk L. Yung
Figure caption: Same as Figure 2, except the length of the time series is 4 days. The 99% confidence threshold in panel (d) is lower than the threshold in Figure 2(d) due to the shorter time series.
Paper: Rotation Period Detection for Earth-like Exoplanets
Authors: Jiazheng Li, Jonathan H. Jiang, Huanzhou Yang, Dorian S. Abbot, Renyu Hu, Thaddeus D. Komacek, Stuart J. Bartlett, Yuk L. Yung
Figure caption: The flowchart of the algorithm that is used to determine whether the rotation period of the exoplanet can be detected from a simulated time series.
Paper: On the Same Wavelength as the Space Telescope Imaging Spectrograph
Authors: Thomas R. Ayres
Figure caption:                         Wavelength residuals, in equivalent velocities. “Cx” (top panel) refers to standard CALSTIS; “Cz” (second from top) is Cx corrected during post-processing with a third-order polynomial in λ; “Ax” (second from bottom) denotes processing by CALSTIS with ASTRAL reference files, including updated dispersion coefficients; and “Az” (bottom panel) is Ax corrected post-facto by an ASTRAL distortion map. Numerical values in the titles are the standard deviations of the residuals around the zero line, illustrated by horizontal red dashed lines (±1σ) in the individual panels. These comparisons are for single wavecal exposures, rather than the co-added spectra of Figures 3, thus the standard deviations for the Cx cases can differ from the bracketed values in Table 3. The secondary settings are noted in a dark font; the one primary is in red. (a) FUV secondary setting E140H-1562; (b) NUV secondary setting E230H-1863; (c) NUV primary setting E230H-2762.
Paper: On the Same Wavelength as the Space Telescope Imaging Spectrograph
Authors: Thomas R. Ayres
Figure caption: Wavelength residuals and fitted models for the twelve supported primary STIS echelle settings. Each panel depicts λ obs − λ lab, expressed as equivalent velocities, as a function of wavelength. The y-axis scales correspond roughly to ±1 resel. The smooth dashed curve is a polynomial of degree 3, or higher in some cases. The faintly visible gray-scale image behind the points is a probability density map representing uncertainties of the fit. Yellow circled dots are excluded ≥3σ outliers. (a) Single prime CENWAVE for FUV-M and the three for FUV-H; (b) the two prime CENWAVEs for NUV-M, and the leading two for NUV-H; (c) the final four NUV-H primes.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: CO line kinematics for different components (marked in different colors as shown in the legend, with absorption components in green), by combining the iSHELL and CRIRES surveys. Symbols reflect the full line shape parameter S as in Figure 6. The FWHM of individual emission components overall increases with the disk inclination and decreases with the stellar mass and infrared index. CO line centroids predominantly show small blueshifts, in both the emission and absorption components.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: CO line excitation for different components, by combining the iSHELL and CRIRES surveys. Symbols reflect the full line shape parameter S as in Figure 6. The ratio of high-J to low-J v = 1 − 0 lines, a proxy for the rotational excitation, increases with the line FWHM (left). Absorption components generally have values <0.1 and are not included for better visualization of the trend. The v2/v1 ratio, a proxy for vibrational excitation, shows grouping of data points according to their FWHM as will be discussed in Section 5 (middle). The 12CO/13CO ratio, a proxy for column density, increases with the line FWHM. In these three excitation tracers, absorption components, especially those measured in highly inclined disks, show measurements that overlap with those obtained for the emission components, especially in NC. These three excitation tracers show no global relation to the stellar or accretion luminosities (Appendix E).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: CO line shape parameter S as a function of T eff, disk inclination, and infrared index for the iSHELL (black) and CRIRES (orange) surveys combined. Top row: Representative line shapes from Figure 5 are separated into “triangular” to the left (S ≳ 2.5, triangle symbols) and double-peaked to the right (S ≲ 2.5, square symbols); the measured shape parameter S (Section 4.2) is included in each plot at the top left. Line profiles are labeled with letters to identify different regions in the parameter space below. Bottom row: Triangular lines are more frequent in T Tauri systems while double-peak lines in Herbig AeBe disks (left plot). Both line types are observed at all disk inclinations in both disks with and without an inner cavity (middle and right plots). Geometric effects for gas in Keplerian rotation (dashed lines; Bast et al. 2011) and self-absorption from a wind (solid line; Pontoppidan et al. 2011) are shown for reference in the middle plot.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Overview of line shapes observed in the iSHELL survey, showing line stacks for 12CO v = 1 − 0 J = 5–18 (black), v = 1 − 0 J = 25–31 (orange), v = 2 − 1 (purple), 13CO v = 1 − 0 (green). Double-peak lines are shown in the top half of the figure, triangular lines in the bottom half. CO is only marginally detected in emission in HD 145718, which is included at the end for reference. 51 Oph is not included because the stacked line profiles cannot be reliably extracted due to the extremely broad FWHM. The vertical dashed and dotted lines shows the stellar RV and its uncertainty. The measured line shape parameter S is reported at the top right in each plot. The corresponding figure for targets in the CRIRES survey is reported in the Appendix.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Overview of kinematic variability observed in CO v = 1 − 0 emission lines. Epochs are written in each plot in the format mmmyy (three letters for the month, two numbers for the year). Spectra from 2007 to 2008 have been taken with CRIRES (Pontoppidan et al. 2011; Brown et al. 2013) and those from 2016 to 2021 with iSHELL (this work). Double-peak line shapes are shown at the top of the figure, followed by triangular lines below. In the case of HD 163296, the second spectrum is taken two days later with the 0.″75 slit (Appendix F); this target is included in this figure for reference to kinematic variability observed before in Hein Bertelsen et al. (2016b).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Examples of stacked lines and of line decomposition into BC and NC where present. The vertical dotted line marks the line center for reference. Top: example of a spectrum with a single-component, double-peak line shape. Middle and bottom: examples of triangular lines with two CO components, BC marked in red and NC marked in blue (the dashed line shows NC on its own, the solid line shows NC as summed to BC). AS 205 N is an example where the two components can be well described with Gaussian functions, while RNO 90 is an example where the v = 2 − 1 line profile is used to define BC (as in Banzatti & Pontoppidan 2015).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Sample comparison between this iSHELL survey and a previous survey done at similar resolving power with VLT-CRIRES (Pontoppidan et al. 2011; Brown et al. 2013, see Section 2.1). The third plot to the right reports detection rates for 12CO v = 1 − 0 emission, 13CO v = 1 − 0 emission, CO lines in absorption, “triangular” line shapes, and Keplerian line shapes (see Section 4.2 for line shapes definitions).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Overview of v = 1 − 0, J = 1 absorption lines (black: 12CO, green: 13CO). The spectra are shown after subtraction of CO emission (some residuals from imperfect subtraction are visible in V892 Tau). The vertical dashed and dotted lines shows the stellar RV and its uncertainty.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: iSHELL resolving power with the two slits used in this survey, as estimated from Gaussian fits to narrow CO absorption lines.
Paper: The Perkins INfrared Exosatellite Survey (PINES) I. Survey Overview, Reduction Pipeline, and Early Results
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, David Gracia, Johanna M. Vos, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty, Christopher Theissen, Eric Agol, Julie N. Skinner, Sheila Sagear
Figure caption: Spitzer light curves for the variable brown dwarf SIMP 1629+0335. The top panel displays the data taken in Channel 1 (3.6 μm) in 2012. The middle and bottom panels display the data from Channel 2 (4.5 μm) and Channel 1 (3.6 μm), respectively, taken in 2015. The corrected light curves are shown in red, with 50 random draws from our MCMC fit shown in black. The measured rotation period is significantly different in all three epochs.
Paper: The Perkins INfrared Exosatellite Survey (PINES) I. Survey Overview, Reduction Pipeline, and Early Results
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, David Gracia, Johanna M. Vos, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty, Christopher Theissen, Eric Agol, Julie N. Skinner, Sheila Sagear
Figure caption: Variability recovery for SIMP 1629+0335. Top: PINES observations taken in J band with a 60 s exposure time. The 60 s exposures are shown in gray, while the data binned over 8 minutes blocks are shown in black with error bars. Middle: a Lomb-Scargle periodogram of the unbinned data. Bottom: photometry with random MCMC models overplotted.
Paper: The Perkins INfrared Exosatellite Survey (PINES) I. Survey Overview, Reduction Pipeline, and Early Results
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, David Gracia, Johanna M. Vos, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty, Christopher Theissen, Eric Agol, Julie N. Skinner, Sheila Sagear
Figure caption: PINES light curve of the new variable WISE J0457−0207. We estimate its variability period to be 5.748 hr. The panels match those in Figure 12.
Paper: The Perkins INfrared Exosatellite Survey (PINES) I. Survey Overview, Reduction Pipeline, and Early Results
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, David Gracia, Johanna M. Vos, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty, Christopher Theissen, Eric Agol, Julie N. Skinner, Sheila Sagear
Figure caption: PINES light curve of the known variable 2MASS 2139+0220. The panels match those in Figure 12.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: Results of FoF testing in Illustris when varying the linking length (top), probability cutoff (middle), and photometric redshift uncertainty cutoff (bottom). The solid gold vertical lines represent the parameter value selected for the FoF algorithm in all three cases. The blue lines show how the fraction of groups with 100% completeness (solid) and over 70% completeness change as the parameter is varied, while the red lines show how the fraction of groups with 0% false positives (solid) and less than 30% false positives (dashed) change as the parameter is varied. Parameters were selected by balancing the completeness and false-positive rate as much as possible. In these plots, the parameters that were held constant were the final parameters while the third was varied.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: Absolute r-band magnitude as a function of photometric redshift for the bent and unbent samples, as well as all identified group members. The blue line signifies an r = 21 limiting apparent magnitude. The majority of radio galaxies are below an absolute magnitude of −22, making up the brightest galaxies. It is important to note that only galaxies below z = 0.5 are considered in this study.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: (Top) A 2D histogram from DECaLS galaxies of the photometric redshift uncertainty as a function of apparent r-band magnitude. (Bottom) A Gaussian Kernel Density Estimate (KDE) of the top plot. In both plots, the red dashed line represents an uncertainty of 0.04, which is what we have chosen as our redshift uncertainty cutoff. This results in many fainter (r > 20) galaxies being excluded from this analysis, as can be seen in Figure 4.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: The distribution of 3D distances to the nearest neighbor for all galaxies in groups of at least five members in the Illustris TNG300 simulations. This histogram only takes into account galaxies that would be observable by DECaLS at a redshift of roughly z = 0.1. The vertical lines show different characteristics of this distribution that were tested as linking lengths for our FoF algorithm.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: The 3σ contours from FIRST plotted over DECaLS r-band images, all of which are 2 by 2 arcminutes on each side. The red circle indicates the position of the host galaxy in SDSS. Left side: Two examples of bent doubles. Right side: Two examples of unbent AGN.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: The distribution of FIRST integrated fluxes for the bent and unbent samples.
Paper: How Does Environment Affect the Morphology of Radio AGN?
Authors: Melissa Elizabeth Morris, Eric Wilcots, Eric Hooper, Sebastian Heinz
Figure caption: Normalized histograms comparing the redshift distributions of bent and unbent AGN in our sample.