adsabs/AstroCLIMB huggingface dataset:
Paper: Imaging the Milky Way with Millihertz Gravitational Waves
Authors: Kaitlyn Szekerczes, Scott Noble, Cecilia Chirenti, James Ira Thorpe
Figure caption: False-color image of simulated LISA (top) and AMIGO (bottom) detections of UCB binaries with one year of data. The size of the median CDL, ﹩\bar{\mathrm{CDL}}﹩, over all sources is represented by a red circle in each image.
Paper: Imaging the Milky Way with Millihertz Gravitational Waves
Authors: Kaitlyn Szekerczes, Scott Noble, Cecilia Chirenti, James Ira Thorpe
Figure caption: Spectral density of gravitational-wave luminosity for the simulated observations of UCBs with LISA. Luminosity is expressed as relative intensity computed using (4). The gistrainbow colormap from matplotlib is used to color the frequency bins so that the colors match those used in the images below.
Paper: Imaging the Milky Way with Millihertz Gravitational Waves
Authors: Kaitlyn Szekerczes, Scott Noble, Cecilia Chirenti, James Ira Thorpe
Figure caption: False-color image of LISA detections of 10026 UCB binaries from a high-fidelity simulation of source identification and extraction using GBMCMC as described in Lackeos et al. (2023). Compare with the image made using the coherent diffraction limit in Figure 4.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The (intrinsic) absolute magnitude distribution from the modified base model where we extended the model domain to 15 < H < 28 (solid black line). The gray area shows the 99.7% envelope of posteriors from the MultiNest fit. For reference, we also plot the magnitude distributions from Harris & D’Abramo (2015; green line), Granvik et al. (2018; dashed black line for 17 < H < 25), Harris & Chodas (2021; red line), and Heinze et al. (2021; blue line). Note that the vertical blue bar at H = 28 shows the 1σ uncertainty reported in Heinze et al. (2021) for the number of NEO with H < 28.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The impact flux on the terrestrial planets as a function of NEO absolute magnitude. The black, green, blue, and red lines show the impact flux for Mercury, Venus, Earth, and Mars. The thin solid lines near the Earth flux are the base-model NEO magnitude distribution scaled with the fixed impact probability (1.5 × 10−3 Myr−1; see the main text). The thin solid line near the Mars flux is the Earth profile scaled down by a factor of 3. The horizontal dashed line shows the impact flux for D > 1 km bodies from Morbidelli et al. (2020; 0.75 Myr average spacing between impacts). The vertical dashed line corresponds to H = 17.75.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The impact flux on the terrestrial planets as function of NEOs absolute magnitude. The black, green, blue, and red lines show the impact flux for Mercury, Venus, Earth, and Mars, respectively, from Equation (13). The thin solid line near the Earth flux is the NEO magnitude distribution from Harris & Chodas (2021) scaled with the fixed impact probability (1.5 × 10−3 Myr−1; see the main text). The black dot approximately marks the constraint from bolide detonations in the Earth atmosphere (Brown et al. 2002). The horizontal dashed line shows the impact flux for D > 1 km bodies from Morbidelli et al. (2020; 0.75 Myr average spacing between impacts). The vertical dashed line corresponds to H = 17.75.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The incompleteness of the known PHO population (MOID <0.05 au, H < 22). For the a, e, and i distributions, the dashed lines show the number of known PHOs with H < 22, and the solid lines are the number of PHOs with H < 22 inferred from our maximum likelihood base model (both given per bin interval; 0.1 au, 0.°04 and 4°). For the H distribution in the bottom-right panel, we show both the cumulative and differential (per 0.25 mag) distributions (upper and lower lines, respectively; solid for model, dashed for known). The uncertainty of the cumulative population estimates increases from ≃3% for H < 20 to ≃6% for H < 25. The uncertainties were obtained from the posterior distribution produced by MultiNest and do not account for various uncertainties of the CSS detection efficiency.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The probability PDFs of a, e, i, and H from our modified base model with the extended magnitude range (15 < H < 28; blue lines) is compared to the CSS NEO detections (red lines). The shaded areas are 1σ (bold gray), 2σ (medium), and 3σ (light gray) envelopes. We used the best-fit solution (the one with the maximum likelihood) from the modified base model and generated 30,000 random samples with 4412 NEOs each (the sample size identical to the number of CSS’s NEOs in the model domain; 15 < H < 28). The samples were biased and binned. We identified envelopes containing 68.3% (1σ), 95.5% (2σ), and 99.7% (3σ) of samples and plotted them here.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The incompleteness of the known NEO population. For the a, e, and i distributions, the dashed lines show the number of known NEOs with H < 22, and the solid lines are the number of NEOs with H < 22 inferred from our maximum likelihood base model (both given per bin interval; 0.1 au, 0.°04, and 4°). For the H distribution in the bottom-right panel, we show both the cumulative and differential (per 0.25 mag) distributions (upper and lower lines, respectively; solid for model, dashed for known). The uncertainty of the cumulative population estimates increases from ≃3% for H < 20 to ≃6% for H < 25. The uncertainties were obtained from the posterior distribution produced by MultiNest and do not account for various uncertainties of the CSS detection efficiency.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The PDFs of a, e, i, and H from the intrinsic (debiased) base model. The plot compares the distributions of bright NEOs with 15 < H < 17.5 (blue) and faint NEOs with 22.5 < H < 25 (red). The blue and red shaded areas are the 1σ envelopes of our base model posteriors.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: A sample output from the NEOMOD Simulator that shows ≃4.1 × 105 orbits of NEOs with H < 25.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: V451 Oph: the difference between the composite model and the spectrum. The differences from models of six T 1 temperatures (indicated in the figure) are shown from top to bottom. An arbitrary constant has been added to the difference spectra so that they do not overlap. (T 2 fixed at 9800 K.) The best fit is indicated with a black line. The changes as a function of model temperature are clear in the comparison. The coolest model (top) is too low in flux for the shorter wavelengths as compared with the (normalized) longer wavelengths. Conversely, for a hotter model (bottom) the model fluxes are larger than the spectrum for wavelengths shorter than 1300 Å. In this temperature range, the poor agreement in the Lyα region near 1200 Å is particularly marked for the hottest model.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: V451 Oph: comparison of the IUE unreddened spectrum and models. Lines are: IUE spectrum: black; hot model: green; cool spectrum: blue; model composite: red. Model T 1 (hot) temperatures are indicated in each panel. The best fit is for T 1 = 12,000 K. Wavelength is in Å; flux is in erg cm−2 s−1 Å−1 in all figures.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: Log-R vs. log-M relation from the TAG sample. Main-sequence stars are in black; other stars are in red. The group of other stars includes χ 2 Hya, Group III stars, and Am stars (see text). Masses are in M ⊙; radii are in R ⊙.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: V451 Oph: the temperature determination: the standard deviation as a function of temperature of the primary. The temperature of the secondary was fixed at 11,000 K; dots: the standard deviation from the spectrum-model comparison; triangles: the parabola fit.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: The mass–temperature relation. Main-sequence stars are in black; others are in red. Others include χ 2 Hya, Group III stars, and Am stars. Masses are in M ⊙; temperatures are in K.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: YZ Cas: comparison of IUE spectrum and models. Lines are the same as in Figure 1. The magenta line above the spectrum in the upper left at 1550 Å indicates that this feature was not included in the fit. Best fit is for T 1 = 9000 K.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: YZ Cas: the temperature determination: the standard deviation as a function of temperature of the primary. The temperature of the secondary was fixed at 7250 K; dots: the standard deviation from the spectrum-model fit; triangles: the parabola fit.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: YZ Cas: the difference between the model and the IUE spectrum. The differences from models of five temperatures is shown from top to bottom with increasing model temperature. The best fit is indicated with a black line.
Paper: The Mass–Temperature Relation for B and Early A Stars Based on International Ultraviolet Explorer Spectra of Detached Eclipsing Binaries
Authors: Nancy Remage Evans, Mckenzie G. Ferrari, Joanna Kuraszkiewicz, Steven Silverberg, Joy Nichols, Guillermo Torres, Makenzi Fischbach
Figure caption: The temperatures from the IUE spectral fit log T(IUE) vs. the temperatures from TAG log T(TAG). Both temperatures are in K.
Paper: OGLE-2016-BLG-1195 AO: Lens, Companion to Lens or Source, or None of the Above?
Authors: Andrew Gould, Yossi Shvartzvald, Jiyuan Zhang, Jennifer C. Yee, Sebastiano Calchi Novati, Weicheng Zang, Eran O. Ofek
Figure caption: Offsets in the positions of two nearby stars relative to that of the microlensed source (black) as determined from a difference imaging analysis of KMT data from the microlensing event in 2016. The two stars lie in the northwest and southeast quadrants of the zoom of Figure 1 from Vandorou et al. (2023). The analysis of the present work yields the offsets of these two stars at two epochs, i.e., 2018 (blue, NIRC2) and 2020 (red, OSIRIS). The northwest star is much closer to the microlensed source, suggesting that the two are associated. By contrast, Vandorou et al. (2023) assumed that the southeast star was associated with the microlensing event. Note that the black error bars reflect the precision of centroiding the source within the KMT difference images, whereas the blue and red error bars reflect the precision of transforming from the Keck images to the KMT reference image. As discussed in the text, we estimate the true centroiding errors to be ∼15 mas; for reference, we show ±15 mas error bars in yellow to the lower right of the plot.
Paper: OGLE-2016-BLG-1195 AO: Lens, Companion to Lens or Source, or None of the Above?
Authors: Andrew Gould, Yossi Shvartzvald, Jiyuan Zhang, Jennifer C. Yee, Sebastiano Calchi Novati, Weicheng Zang, Eran O. Ofek
Figure caption: Positions of the 20 brightest stars (in I band) from the KMTC01 pyDIA reduction that overlap the Keck OSIRIS image (solid rectangle). The star positions are in the original reference-frame pixel coordinates. The pixels are approximately ﹩{0.4}^{{\prime} ^{\prime} }﹩. For ease of comparison to the Keck images, the stars are color coded according to K pseudo ≡ I − (V − I) by K pseudo < (13, 13.5, 14, 14.5, 15, 15.5) → (black, red, green, cyan, blue, magenta). The source position (X, Y)source=(153.074, 150.317) is shown by a cross.
Paper: OGLE-2016-BLG-1195 AO: Lens, Companion to Lens or Source, or None of the Above?
Authors: Andrew Gould, Yossi Shvartzvald, Jiyuan Zhang, Jennifer C. Yee, Sebastiano Calchi Novati, Weicheng Zang, Eran O. Ofek
Figure caption: Caustic geometries for the four solutions shown in Table 2 and illustrated in Figure 3. In the “central-caustic” models, the “bump” in the light curve centered at 7569.13 is caused by the source passing over a ridge that extends from the central (or resonant) caustic, whereas in the “resonant-caustic” models, it is caused by the source passing over two closely spaced caustics of the planetary wing of a resonant caustic.
Paper: OGLE-2016-BLG-1195 AO: Lens, Companion to Lens or Source, or None of the Above?
Authors: Andrew Gould, Yossi Shvartzvald, Jiyuan Zhang, Jennifer C. Yee, Sebastiano Calchi Novati, Weicheng Zang, Eran O. Ofek
Figure caption: Keck images of the region surrounding OGLE-2016-BLG-1195 from OSIRIS 2020 (left) and NIRC2 2018 (right). In each case the position of the microlensed source (in the 2016 bulge frame) is superposed as a blue circle. The pixel sizes are, respectively, 10 and 40 mas. North is up and east is left. Vandorou et al. (2023) identified the southeast star (or asterism) as the location of the microlensing event, whereas our analysis suggests that this is more likely to be the northwest star.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: TESS light curve for asteroid 135886 in instrumental magnitudes corrected for distance and phase angle (i.e., “absolute” instrumental magnitudes). The rotational phase of the object is scaled from zero to P, where P is the derived rotation period of the object.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Histogram showing the number of observations per object across TESS Cycle 1. The y-axis in this figure shows the raw number of objects in each bin.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Plot of rotation period against diameter for all objects in the LCDB with quality code ≥2−. The data are from Warner et al. (2009). Note that the data here are from 2020, before the addition of any other periodicities from TESS.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The LAMOST low-resolution spectra of 16 CTTSs in this study.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The example for demonstrating the examination of the contamination from nearby sources. The left panel is the TPF of GG Tau (TIC 245830955), and GG Tau is marked by a red filled circle. The red open circles are the field stars with G RP < 15 queried from Gaia DR3. The pink mask pixels are the aperture given by the SPOC pipeline. We found that the field star located in the aperture is much fainter than GG Tau, and the overall shapes of light curves from different test apertures do not change significantly compared to the SPOC light curve. Therefore, we verified that the data of GG Tau can be used in this study. The right panel is the TPF of GI Tau (TIC 268444803). There are three neighbor stars within or at the edge of the SPOC aperture, and one of them is equally bright to GI Tau, making it hard to distinguish the variability feature between GI Tau and the neighbor stars in the light curve. As the result, we excluded GI Tau data from the following analysis.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The examples of the period reestimate/estimate of the CTTSs, here showing (a) DL Tau and (b) IQ Tau. In each case, the top left panel shows the autocorrelation function. The gray one is the original ACF, and the blue one is a smoothed version of the ACF. The red cross marks the peak of the ACF, and the FHWM is highlighted by green, from where the best period is determined. The top right panel is the phase curve (black) and the best GP fit curve (red). The panel at the bottom is the full TESS Section 43 and 44 light curve of the star (black) with the best GP fit curve (red). The best periods we found for DL Tau and IQ Tau are 10.4 and 12.9 days, respectively.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: Three examples of the flux calibration processes in this study. The top left panel is AA Tau, the top right panel is DL Tau, and the bottom panel is GO Tau. In each panel, the blue curve represents the star's spectrum, while the gray curve represents its corresponding best-fit template spectrum given by Manara et al. (2013). The photometric data from ASAS-SN g band and V band are marked as a yellow circle in the AA Tau case and a green circle in the DL Tau case, respectively. The Pan-STARRS i-band data of GO Tau are marked as a red circle in the GO Tau panel.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The Q–M statistics diagram for our sample of CTTSs. The stars surrounded by black open circles in this diagram are binary or multistar systems. Different colors represent different variability classes: yellow (B), purple (P), green (QPS), blue (APD), and red (QPD).
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: Hα emission profiles of our targets observed by LAMOST. In each panel, the spectra are displayed in red, and the black line represents the fit local continuum. The dashed vertical line in gray marks the center wavelength of the Hα line.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: Ca II λλ8498, 8542, 8662 emission profiles of our targets observed by LAMOST. Dashed vertical gray lines represent the center of the Ca II triplet lines in each panel.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: a−dHe I λλ4471, 5875, 6678, 7065 emission profiles of our targets observed by LAMOST. Dashed vertical gray lines represent the center of He I in each panel.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The TESS light curves of 12 CTTSs in our sample. Their variability classes are also displayed.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: Hβ emission profiles of our targets observed by LAMOST. Dashed vertical gray lines represent the center of the line in each panel.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The fractional response functions of TESS (red), ZTF r (orange), ZTF g (lightgreen), SDSS g (green), and U bands (blue). They are the function of the blackbody temperature.