adsabs/AstroCLIMB huggingface dataset:
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: A corner plot of a sample full-orbital fit. Note that period and epoch of periastron passage (t 0) are calculated according to Table 2.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Marginal posterior distribution for the orbital parameters of the HIP 89000 binary system in the SB2 and SB1 cases. In each panel, we indicate the MAP estimate for the SB2 and its SB1 analog. Of course, at this stage, we can estimate the orbital parallax, the mass for the primary, and the mass ratio only in the SB2 case. The small dot with 2σ error bars in the pdfs for ϖ and m 1 indicate the values shown in Table 1. For this particular case, the good correspondence between the orbital and trigonometric parallax is evident; this was documented already by Mendez et al. (2017).
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Estimated orbit and RV curves of the HIP 89000 binary system. First column: MAP point estimate projection of the posterior distribution for the SB2 and SB1 cases (note that in the lower left panel, the curves for the SB2 and SB1 cases overlap). Second and third columns: projected posterior distribution of the SB2 and SB1 cases, respectively.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Similar to Figure 2, but for the HIP 111170 binary system. In this case there is a more noticeable difference between the orbital and trigonometric parallaxes, also documented in Mendez et al. (2017), who used the pre-Gaia trigonometric parallax 39.35 ± 0.70 [mas].
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Similar to Figure 1, but for the HIP 111170 binary system.
Paper: Around the Spindle Galaxy: The Dark Halo Mass of NGC 3115
Authors: I. D. Karachentsev, L. N. Makarova, G. S. Anand, R. B. Tully
Figure caption: Color-composed images of five new probable satellites of NGC 3115 taken from the DECaLS survey. The size of the stamps is 2′. North is up and east is left.
Paper: Around the Spindle Galaxy: The Dark Halo Mass of NGC 3115
Authors: I. D. Karachentsev, L. N. Makarova, G. S. Anand, R. B. Tully
Figure caption: Color–magnitude diagrams of the observed galaxies. The TRGB positions are indicated by the horizontal lines. Photometric errors are shown by the bars at the right in the CMDs.
Paper: Around the Spindle Galaxy: The Dark Halo Mass of NGC 3115
Authors: I. D. Karachentsev, L. N. Makarova, G. S. Anand, R. B. Tully
Figure caption: Two-color HST/ACS images of five dwarf galaxies around NGC 3115: UGCA 193, KKSG 17, 2MASX-J0957-0915, 2dFGRS-TGN218Z179, and KKSG 19. North is up and east is left.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Results of error estimation based on simulated light curves (see text for details) for the mean magnitudes obtained with template light-curve fittings. For a better visualization, the g- and i-band data points were offset slightly on the x-axis. The upper panel presents the averaged Δ m  obtained from 1000 simulated light curves as a function of N, the number of data points per light curve. The error bars represent a 1σ standard deviation on the averaged values. The horizontal dashed lines represent 〈Δ m 〉 = 0. The inset in the upper panel is an enlarged version with error bars omitted for clarity. In the lower panel, the corresponding standard deviations were plotted as a function of N. The orange curve in the inset is the best-fit exponential decay function to describe the trend of the standard deviations, at which the fittings of the exponential decay function were only done on data points with N ≥ 10.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Comparison of the amplitudes for the RR Lyrae in our sample (represented in blue, green, and red for the gri bands, respectively) and the RR Lyrae located in the SDSS Stripe 82 region (adopted from Sesar et al. 2010; gold and purple squares). The RR Lyrae in our sample with type RR0 (or RRab) and RR1 (or RRc) are marked with circles and triangles, respectively. The horizontal lines represent the adopted amplitude cuts in each filter, separated for RR0 and RR1, with values given next to these lines (see text for more details).
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Residuals of the fitted PL relations given in Figure 6, in units of the PL dispersion σ, as a function of the light-curve amplitudes. The orange dotted horizontal line represents the zero residuals to guide the eye. The solid horizontal lines are the boundaries on the positive residuals determined using the boundfit code (Cardiel 2009; see text for more details). The dashed horizontal lines are the boundaries on the negative residuals mirrored from the solid horizontal lines. The sizes of these horizontal lines were based on the adopted amplitude cuts (see Figure 3). Upper and lower panels are for RR0 (filled circles) and RR1 (filled triangles), respectively.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: The gri-band amplitude ratios as a function of pulsation period for the RR Lyrae in our sample, marked as filled orange circles and cyan triangles for RR0 and RR1, respectively. The horizontal solid lines represent the amplitude ratios of unity. The dotted lines are the adopted upper limits for the amplitude ratio cuts (see text for more details).
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Residuals of the fitted PW relations given in Figure 8, in units of the PW dispersion σ, as a function of the amplitude ratios. The orange dotted horizontal line represents the zero residuals to guide the eye. The solid horizontal lines are the boundaries on the positive residuals determined using the boundfit code (Cardiel 2009; see text for more details). The dashed horizontal lines are the boundaries on the negative residuals mirrored from the solid horizontal lines. The sizes of these horizontal lines were based on the adopted amplitude ratio cuts (see Figure 4). The upper and lower panels are for RR0 (filled circles) and RR1 (filled triangles), respectively.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Extinction-corrected PC (top three panels) relations and the extinction-free Q-indices as a function of pulsation period (i.e., the PQ relation; bottom panel) for the RR Lyrae in our sample, separated for RR0 (filled orange circles) and RR1 (filled cyan triangles). The red dashed lines indicate the selection boundaries based on the provisional fitted PC/PQ relations to the RR0 and RR1 combined samples (see text for more details).
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Composite gri-band PL relations based on the 1209 RR Lyrae in different globular clusters, separated for RR0 (upper panels) and RR1 (lower panels). The solid lines are the provisional fitted PL relations (see text for details). For clarity, error bars are omitted. The colors of the data points represent the amplitudes derived from the best-fit template light curves.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Composite PW relations based on the 1209 RR Lyrae in different globular clusters, separated for RR0 (upper panels) and RR1 (lower panels). The solid lines are the provisional fitted PW relations (see text for details). For clarity, error bars are omitted. The colors of the data points represent the amplitude ratios derived from the best-fit template light curves.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Venn diagram for the excluded RR Lyrae in our sample (see text for details on flags A, C, and R).
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption:  Left panel: Velocity-integrated [C II] map of the sky region around PSO J083+11. We find a companion galaxy in the southwest direction from the central quasar, with a projected angular separation of 2.″88, or equivalent to ∼16 kpc at z = 6.3309. The ALMA synthesized beam’s size is presented at the bottom left. The solid black lines denote the [C II] velocity-integrated flux contours with [3, 4, 5, 7, 9, 12, 15] ×σ, where σ = 0.053 Jy beam−1 km s−1. Contours with negative values are shown with dashed black lines. For extracting the spectrum and calculating the total [C II] flux density of the companion galaxy, we use a circular aperture (see dotted circles) with a radius of 1″ (equivalent to 5.5 kpc). Right panel: The companion galaxy’s [C II] emission at the observed frequency of ν obs = 259.25 GHz. The observed flux density, its associated ±1σ uncertainty, and the fitted Gaussian model are shown with the blue, dashed gray, and solid red lines, respectively. The velocity axis centered at z = 6.3309 is presented at the top. The expected central wavelengths of [C II] lines from the sub-DLA at z = 6.314 and PSO J083+11 at z = 6.3401 discussed in the main text are marked with the orange and green areas, respectively.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: Spectrum of PSO J083+11 (black line), shot noise (gray line), and associated PCA model (red line and shaded region) around the wavelength region where the quasar’s Lyα emission is expected. The left panel shows the absorption from a z = 6.314 sub-DLA with a hydrogen column density of logN HI = 20.11 ± 0.30 cm−2 (blue line and shaded region). Even though it already gives a good fit, we explore an alternative model to test how much the PSO J083+11’s proximity zone is truncated due to the presence of the aforementioned sub-DLA. The right panel presents a joint model where we incorporated attenuation due to an IGM with ﹩{\overline{x}}_{\mathrm{HI}}=0.1﹩ (orange dashed line) and sub-DLA with ﹩\mathrm{log}{N}_{\mathrm{HI}}=20.03\pm 0.30﹩ cm−2 (green dashed line). This joint IGM + DLA model (blue line and shaded region) reconstructs the data at λ = 1216–1225 Å slightly better, although not significant (see wavelengths marked with green). The residual of the fits (blue circles) and masked wavelengths to avoid strong absorption lines or regions with large uncertainty in the sky subtraction (gray shaded area) are also presented in the figure. See Appendix C for the impact of other ﹩{\overline{x}}_{\mathrm{HI}}﹩ values.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption:  All panels show the observed spectrum of PSO J083+11 (solid black line), its 1σ shot noise vector (gray line), PCA continuum model (red line), and best-fit damping wing model (blue line). In the top left panel, we present the damping wing shape assuming there is zero IGM contribution (i.e., ﹩{\overline{x}}_{\mathrm{HI}}=0.0﹩). The rest of the left panels present the increasing attenuation by the IGM with the sub-DLA Voigt profiles (green dashed lines; see legends) being modeled using the already attenuated quasar continuum (orange dashed lines) as input. The combination (blue line) is the best-fit match for the observed spectrum (solid black lines). The reduced chi-squared (﹩{\chi }_{\mathrm{red}}^{2}﹩) value for each IGM + DLA model is indicated with the blue text. As discussed in Section 3.2, the fiducial model that we choose is a 10% neutral IGM and correspondingly a best-fit sub-DLA profile of ﹩\mathrm{log}{N}_{\mathrm{HI}}=20.03\pm 0.30﹩ cm−2. The right panels show the example cases where the quasar’s proximity zones extend beyond or within the sub-DLA redshifts but still give comparably good fits.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: Pseudo-narrowband images of PSO J083+11 created based on the MUSE data. The black dotted circles mark an aperture with a size of 0.″75 used for extracting the quasar spectrum. In the left panel, we show the pseudo-narrowband image centered on the expected Lyα emission wavelength (λ obs = 8850–8997 Å) as highlighted by the magenta region of the spectrum in the inset of Figure 2. The continuum, and hence point-source image, constructed by collapsing data cube wavelength layers around the quasar continuum emission, is shown in the middle panel. The wavelength range (λ obs = 9100–9200 Å) combined into this image is denoted in green in the inset of Figure 2. Finally, the right panel shows the pseudo-narrowband image centered on the Lyα line after removing the quasar point source with the PSF subtraction procedure explained in Section 4.1. There is no obvious detection of Lyα halo as seen in the point-source-subtracted residual image. As a side note, the bright emission to the south of the central quasar comes from a foreground galaxy located at z ≈ 0.29.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: Corner plot showing posterior distributions of the thermal parameter (T), turbulent parameter (b), and metal column densities listed in Table 1. The inferred b seems biased toward large values while T is highly uncertain (see text). The column densities of Mg II and C II are well constrained because they are clearly detected in the spectrum (see Figure 1). On the other hand, the marginal detection of O I makes its inferred column density has higher error. Nondetections are obvious for Al II and Fe II where their posteriors extend to the minimum value of the input prior. We also adopt the upper limit value for Si II because its presence is not evident in the spectrum.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: MUSE + FIRE spectrum of PSO J083+11 (black line), shot noise (gray line), and the associated PCA model (red line and shaded region) around the wavelength region where the quasar’s Lyα emission is expected. The left panel shows the absorption from a z = 6.314 sub-DLA with a hydrogen column density of ﹩\mathrm{log}{N}_{\mathrm{HI}}=20.23\pm 0.30﹩ cm−2 (blue line and shaded region). The right panel presents a joint model where we incorporated attenuation due to an IGM with ﹩{\overline{x}}_{\mathrm{HI}}=0.8﹩ (orange dashed line) and sub-DLA with ﹩\mathrm{log}{N}_{\mathrm{HI}}=19.66\pm 0.30﹩ cm−2 (green dashed line). This joint IGM + DLA model (blue line and shaded region) reconstructs the data at λ = 1216–1225 Å better (see wavelengths marked with green), but it seems to be unphysical (see text). The residual of the fits (blue circles) and masked wavelengths to avoid strong absorption lines or regions with large uncertainty in the sky subtraction (gray shaded area) are also presented in the figure.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: Relation between metallicity [O/H] and chemical evolution of [C/O]. Measurements for Milky Way stars taken from Fabbian et al. (2009) and Nissen et al. (2014) are marked as gray circles, while low-redshift DLAs (2 ≲ z ≲ 4) from Cooke et al. (2017) are denoted with blue circles. The z ≳ 6 metal-poor DLAs from Bañados et al. (2019) and D’Odorico et al. (2018) are shown with red squares. Specific for the sub-DLA toward PSO J083+11, we show a corrected metallicity where we adopt a correction factor of 0.35 ± 0.35 dex (see text) to account for ionization and depletion effects. Consequently, this changes the measured [O/H] from -2.19 ± 0.44 to -2.54 ± 0.56.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: Azimuthally averaged radial light profile of PSO J083+11’s Lyα emission measured from the PSF-subtracted pseudo-narrowband image. Tentative detection of the halo flux within a 0.″6 aperture radius is observed, but there are no apparent extended Lyα emissions beyond this radius.
Paper: Staring at the Shadows of Archaic Galaxies: Damped Lyα and Metal Absorbers Toward a Young z ∼ 6 Weak-line Quasar
Authors: Irham Taufik Andika, Knud Jahnke, Eduardo Bañados, Sarah E. I. Bosman, Frederick B. Davies, Anna-Christina Eilers, Emanuele Paolo Farina, Masafusa Onoue, Arjen van der Wel
Figure caption: MUSE + FIRE spectrum of PSO J083+11 (black line) and associated shot noise (gray line). The median composite spectrum of the low-redshift quasar analogs is shown as a cyan line with the 1σ dispersion around the median as a light blue region. The PCA model to predict the blue side of the quasar spectrum and its 1σ dispersion are denoted with the red line and shaded region, respectively. The wavelength range and spectrum used in the PCA fit to predict Lyα is shown with the red dashed line. The inset figure shows the zoom-in to the region around Lyα.
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption: Logarithm of the standard deviation of normalized flux for each of our targets. Open circles show the standard deviation of the fully detrended light curves from k2sc (i.e., both pointing systematics and variability have been largely removed), while triangles show light curves detrended only for pointing jitter (i.e., variability is preserved). The solid gray curve illustrates the expected photometric uncertainty based on Poisson photon statistics, a low-level sky background, and a systematic at the 0.15% level. We have shifted this up by a factor of five to produce the dashed gray curve, which we adopt as our threshold for variability detection.