adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: PSF-subtracted images of the observations of ϵ Eridani observations with the JWST/NIRCam coronagraph. Two epochs were observed separated by 6 months to capture the whole disk. Here shown are the images from the full-array mode observations, which were optimized to be sensitive low-mass planets beyond 2″–3″. Sources HST 1 and 2 were previously detected in HST observations (S. G. Wolff et al. 2023), and ALMA 1 by ALMA (M. Booth et al. 2023); source S2 is the only previously undetected source. However, it exhibits an elongated structure indicating that it is likely a background galaxy. Sources S2 and HST 1 disappear during Epoch #1 (left) because they were blocked by the coronagraph optical mount at the edge of the NIRCam detector. The white circle indicated the position of the ALMA disk (M. Booth et al. 2023). The strong noise features appearing east and west are resulting from bright diffraction features associated with the coronagraphic substrate and its mounting plate.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: Mass sensitivities from JWST/NIRCam coronagraphic observations of ϵ Eridani assuming E. F. Linder et al. (2019) model grids. We assume a Jupiter-like planet with log(g) = 3.39, and metallicity equal to the star. Red contours indicate mass estimates for planet b from W. Thompson et al. (2025). A significant part of these contours contain the structured noise resulting from a bright hexpeckles (see Figure 3), which is not accounted for in these curves. The two temperature bounds are chosen according to E. F. Linder et al. (2019) cooling curves shown in their Figure 6.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: Sensitivity limits (5σ) in terms of contrast. The result from these observations with JWST/NIRCam (red and blue) are compared with J. Llop-Sayson et al. (2021) Keck/NIRC2 vortex data. The F444W curve does not include the regions with highly correlated noise associated with the three bright hexpeckles (see Figure 3). The dashed vertical line indicates the inner working angle of the coronagraph.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: Subtraction residuals for each target-PSF pairing used in the high SNR reduction (classic RDI) optimized for the extended emission reduction. Notably, the SGD position #5 is very precisely aligned with Observation #52, resulting in a nearly perfect, residual free subtraction. Images (170 × 170 px) are scaled linearly between −1 and +2 MJy sr−1.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: Full-array observation contrast curves. The exposure time for this mode was optimized for large angular separations (beyond 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5); the subarray mode contrast curve in Figure 3 shows the sensitivity in the inner region.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: Snapshots of spectrum at different points relative to the peak of the Hα light curve. Gray background points are the quiescent spectrum and the solid-colored foreground points are flare excess, taking the observed emission and subtracting the quiescent spectrum to highlight only emission from the flare itself. All velocities are calculated relative to the vacuum wavelength of the transition labeled in each row. From top to bottom, the rows represent different Balmer lines and each column corresponds to different points in time in each column. Each time column is titled with a position relative to the Hα light curve and the time after the start of the observation period in minutes.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: The quiescent APO optical spectrum is plotted in dark blue while the spectrum at flare peak is plotted in orange, with separate panels for the two arms of DIS. The flare only seems to brighten lines relative to the continuum level, leaving the majority of the continuum unchanged. The exception is the continuum below 4500 Å, which appears slightly enhanced. A subset of the optical lines analyzed in this work have been highlighted with ion labels above the line peak.
Paper: Dense-photometry Validation of Superfast-rotating Asteroid Candidates
Authors: Bojan Novaković, Pedro J. Gutiérrez
Figure caption: Spin period vs diameter of asteroids from the LCDB. In the upper panel, all data are shown regardless of quality code. The orange points mark periods with U ≥ 2−, while the black dots are objects with the lower quality code. The lower panel shows only data with highly reliable spin periods (blue dots), including less than 4500 asteroids having a quality code U = 3. In both panels, the green rectangle shows the intervals where targets of this work are located based on their available spin periods. The horizontal red lines show the spin barrier at P = 2.2 hr.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: The quiescent HST FUV spectrum is plotted in dark blue, while the spectrum at flare peak is plotted in orange. The flare spectrum has not been staggered by multiplying a constant factor, but the offset is a physical consequence of the flare brightening the FUV spectrum across the observation bandpass. A subset of the FUV lines analyzed in this work have been highlighted with ion labels above the line peak.
Paper: Dense-photometry Validation of Superfast-rotating Asteroid Candidates
Authors: Bojan Novaković, Pedro J. Gutiérrez
Figure caption: The light curves of 15 asteroids observed in our campaign and the corresponding FALC fits of the data. The horizontal dashed lines mark the midpoints of the light curves.
Paper: Dense-photometry Validation of Superfast-rotating Asteroid Candidates
Authors: Bojan Novaković, Pedro J. Gutiérrez
Figure caption: The histogram of quality codes for rotational periods of asteroids from the LCDB.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: FFDs in equivalent duration space (including uncertainties) for TESS data of EV Lac (blue dots) and GJ 4334 (red triangles) show significant overlap. GJ 4334 appears to exhibit an excess of very large flares relative to EV Lac despite their similar physical properties and slower rotation. The prevalence of large flares also flattens the apparent slope of the FFD for GJ 4334. The results of our regression analysis (see text) are shown as shaded swaths for the central 68% confidence interval on the best fit cumulative FFD (Equation (5)).
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: Light curves of the data and model fits for Balmer series, Ca II K, Lyα, Si IV 1394 Å, and C II 1334/5 Å. The inset panels on the top zoom into the flare onset (left) and flare peak (right) times to show the relative timing of the flare profiles of these lines. There is a trend in the flare onset of the Balmer series, with higher order lines starting first and a delay in the peak of Ca II K relative to the other optical lines. The FUV lines all rise and peak at the same time within uncertainties, but the onset and peak of the FUV lines are both within the onset–peak interval of the optical lines.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: A collection of flare profiles for FUV lines showing the contributions from both the primary peak (orange) and secondary bump (dark gray) with residuals in the bottom panel of each subfigure. The residuals show a hint of quasiperiodic oscillations, but we could not identify a statistically significant peak in a periodogram. The shapes and size of the secondary bump relative to the primary peak differ significantly among these four lines as well as the other FUV lines available in the figure set.
Paper: FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Aylin García Soto, Zachory K. Berta-Thompson, Allison Youngblood, Kevin France, Elisabeth R. Newton, Keivan G. Stassun
Figure caption: A comparison of total equivalent durations across most of the lines, ranging from nearly 1000–30,000 s.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: Log-uniform orbit fitting with orvara: (Left) Predicted orbits with most likely orbit in black along with 100 randomly selected orbits (color coded by mass) from the MCMC posterior distribution. Blue circles show our data, while empty circles show predicted location per epoch. (Center) Position angle versus epoch (right) separation versus epoch
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: No-RV orbit fitting with orvara: (Left) Predicted orbits with the most likely orbit in black along with 100 randomly selected orbits (color coded by mass) from the MCMC posterior distribution. Blue circles show our data, while empty circles show predicted location per epoch. (Center) Position angle versus epoch (right) separation versus epoch
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: The predicted astrometric motion in R.A. (left) and decl. (right) for the the flat prior without RV data. Shown are 100 randomly selected orbits (color coded by mass) from the MCMC posterior distribution and our data with blue circles.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: The predicted astrometric motion in R.A. (left) and decl. (right) for the log-uniform prior. Shown are 100 randomly selected orbits (color coded by mass) from the MCMC posterior distribution and our data with blue circles.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: The predicted astrometric motion in R.A. (left) and decl. (right) for the flat prior. Shown are 100 randomly selected orbits (color coded by mass) from the MCMC posterior distribution and our data with blue circles.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: Predicted location of HIP 99770 b without RV data from the best-fitting orvara orbits (assuming flat priors on the companion mass) in 2028 January.
Paper: Multi-band Spectral and Astrometric Characterization of the HIP 99770 b Planet with SCExAO/CHARIS and Gaia 
Authors: Danielle Bovie, Thayne Currie, Mona El Morsy, Brianna Lacy, Masayuki Kuzuhara, Jeffrey Chilcote, Taylor L. Tobin, Olivier Guyon, Tyler D. Groff, Julien Lozi, Sebastien Vievard, Vincent Deo, Frantz Martinache, Yiting Li, Motohide Tamura
Figure caption: Predicted location of HIP 99770 b from the best-fitting orvara orbits (assuming log-uniform priors on the companion mass) in 2028 January.
Paper: No Giant Planets in the Eta Cassiopeiae System: Dynamical Implications of a Wide Binary Companion
Authors: Stephen R. Kane, Zhexing Li, Michelle L. Hill, Skylar D'Angiolillo, Benjamin J. Fulton, Andrew W. Howard
Figure caption: Results of the injection-recovery test to assess the sensitivity of our RV data to planetary signatures as a function of planetary mass (﹩{M}_{p}\sin i﹩) and semimajor axis (a). The blue dots indicate successfully recovered injected planetary signatures and the red dots indicate unrecovered planets. The color scale corresponding to the probability contours of detecting a planet of a given mass and semimajor axis is shown on the right vertical axis.
Paper: No Giant Planets in the Eta Cassiopeiae System: Dynamical Implications of a Wide Binary Companion
Authors: Stephen R. Kane, Zhexing Li, Michelle L. Hill, Skylar D'Angiolillo, Benjamin J. Fulton, Andrew W. Howard
Figure caption: Results of the dynamical simulation for the Eta Cas system as a function of semimajor axis of the injected planet. The top panel provides the percentage survival calculations for the planet, and the bottom panel shows the maximum eccentricity of the planet. The extent of the HZ is shown in green, where the light green and dark green regions indicate the CHZ and OHZ, respectively.
Paper: No Giant Planets in the Eta Cassiopeiae System: Dynamical Implications of a Wide Binary Companion
Authors: Stephen R. Kane, Zhexing Li, Michelle L. Hill, Skylar D'Angiolillo, Benjamin J. Fulton, Andrew W. Howard
Figure caption: The RV data for Eta Cas plotted against the observation time, including data from the APF, HIRES, Hamilton, and NEID instruments (see details in Section 3.1). We include a linear fit to the observed RV trend caused by the binary orbit.
Paper: No Giant Planets in the Eta Cassiopeiae System: Dynamical Implications of a Wide Binary Companion
Authors: Stephen R. Kane, Zhexing Li, Michelle L. Hill, Skylar D'Angiolillo, Benjamin J. Fulton, Andrew W. Howard
Figure caption: Power spectrum from a frequency analysis of the RV data shown in Figure 1. Significant observational alias locations (diurnal, lunar, annual) are shown as vertical dashed lines.
Paper: The Effect of Offsets from True Orbital Parameters on Exoplanet High-resolution Transmission Spectra
Authors: Yasmine J. Meziani, Laura Flagg, Jake D. Turner, Emily K. Deibert, Ray Jayawardhana, Adam B. Langeveld, Ernst J. W. de Mooij
Figure caption: The top, middle, and bottom panels show GRACES transmission spectra of WASP-76b around the ionized calcium triplet at 849.8 nm, 854.2 nm, and 866.2 nm, respectively. The points represent the binned transmission spectra, while the dotted lines show Gaussian fits to each line profile. Each panel displays results using the ephemeris from either D. Ehrenreich et al. (2020) or E. S. Ivshina & J. N. Winn (2022). The velocity offset refers to the difference in the measured line centers resulting from the use of these two ephemerides.
Paper: The Effect of Offsets from True Orbital Parameters on Exoplanet High-resolution Transmission Spectra
Authors: Yasmine J. Meziani, Laura Flagg, Jake D. Turner, Emily K. Deibert, Ray Jayawardhana, Adam B. Langeveld, Ernst J. W. de Mooij
Figure caption: The figure above illustrates the relationship between velocity offset and angle of periastron for an assumed eccentricity of zero (e = 0). Each line represents the relationship between velocity offset and angle of periastron for different true eccentricity offset. Angles of periastron at ﹩\frac{\pi }{2}﹩ and ﹩\frac{3\pi }{2}﹩ correspond to zero velocity offset, consistent with exoplanet conventions.
Paper: The Effect of Offsets from True Orbital Parameters on Exoplanet High-resolution Transmission Spectra
Authors: Yasmine J. Meziani, Laura Flagg, Jake D. Turner, Emily K. Deibert, Ray Jayawardhana, Adam B. Langeveld, Ernst J. W. de Mooij
Figure caption: Similar to Figure 7, but for the sodium doublet at 589.0 and 589.6 nm. Using the updated ephemeris from E. S. Ivshina & J. N. Winn (2022), we detect blueshifted features with velocity offsets of −1.2 ± 3.3 km s−1 and −1.5 ± 2.3 km s−1, respectively.
Paper: LAMOST Medium-resolution Spectroscopic Survey of the Rosette Nebula
Authors: Li-Yue Zhang, Chao-Jian Wu, Xuan Fang, Wei Zhang, Juan-Juan Ren, Jian-Jun Chen, Hong Wu
Figure caption: Panel (a) illustrates the spatial distribution of the ratio of the [N II]/Hα emission line intensities. A pronounced increase in the line ratios is observed in the northwestern regions. Panel (b) presents the intensity ratios along the three designated cuts depicted in panel (a), in which the zero degree matches the center of the OB cluster NGC 2244. Notably, the increase in the intensity ratio in the northwestern direction occurs at a consistent distance from the central cluster.
Paper: LAMOST Medium-resolution Spectroscopic Survey of the Rosette Nebula
Authors: Li-Yue Zhang, Chao-Jian Wu, Xuan Fang, Wei Zhang, Juan-Juan Ren, Jian-Jun Chen, Hong Wu
Figure caption: The spatial distribution of 12+﹩\mathrm{log}[{\rm{O}}\,{\rm{III}}]/{\rm{H}}\beta ﹩ of the Rosette Nebula, overlaid with the locations of YSOs adopted from the literature (see text in Section 4.2). A significant concentration of YSOs is noticeable in the central region of the nebula. However, the distances to these YSOs are still not yet clear.
Paper: LAMOST Medium-resolution Spectroscopic Survey of the Rosette Nebula
Authors: Li-Yue Zhang, Chao-Jian Wu, Xuan Fang, Wei Zhang, Juan-Juan Ren, Jian-Jun Chen, Hong Wu
Figure caption: The histogram (panel (a)) and the spatial distribution (panel (b)) of [S II]/Hα emission line intensities. Within the optical boundary of the nebula, the values of [S II]/Hα are smaller than 0.3.
Paper: LAMOST Medium-resolution Spectroscopic Survey of the Rosette Nebula
Authors: Li-Yue Zhang, Chao-Jian Wu, Xuan Fang, Wei Zhang, Juan-Juan Ren, Jian-Jun Chen, Hong Wu
Figure caption: The histogram (panel (a)) and spatial distribution (panel (b)) of ionization fraction measured with S+/S ratio.
Paper: The Importance of Standardizing Spectra in the Era of Large Spectroscopic Surveys: A Case Study of M Dwarfs in SDSS-V
Authors: Ilija Medan, Zachary Way, Bárbara Rojas-Ayala, Guy S. Stringfellow, Conor Sayres, Keivan G. Stassun, Andrew R. Casey, Sébastien Lépine, Emma Galligan, Diogo Souto, Andrew K. Saydjari
Figure caption: Top panel: the median-normalized BOSS spectra of the same M dwarf observed at different epochs. The BOSS spectra shown were reduced using v6_2_0 of the BOSS pipeline and include data up until MJD = 60715 (2025 February 9). The dashed black line shows the median-normalized Gaia XP spectrum of the star, for reference. Middle panel: the estimated fraction of flux entering the fiber for each observation of the M dwarf shown in the top panel. Bottom panel: the median-normalized BOSS spectra from the top panel after dividing by the fractional flux curves in the middle panel. The dashed black line shows the median-normalized Gaia XP spectrum of the star, for reference.
Paper: The Importance of Standardizing Spectra in the Era of Large Spectroscopic Surveys: A Case Study of M Dwarfs in SDSS-V
Authors: Ilija Medan, Zachary Way, Bárbara Rojas-Ayala, Guy S. Stringfellow, Conor Sayres, Keivan G. Stassun, Andrew R. Casey, Sébastien Lépine, Emma Galligan, Diogo Souto, Andrew K. Saydjari
Figure caption: H-R diagram of the number of spectra observed with BOSS for the Milky Way Mapper (MWM) during SDSS-V until MJD = 60715 (2025 February 9). The top and right histograms show the cumulative distributions of in G – RP and MG, respectively. For the MG distribution, the location of main-sequence spectral types as a function of MG from M. J. Pecaut & E. E. Mamajek (2013) are shown for reference. From the MG cumulative distribution on the right, an impressive ∼one-third of BOSS MWM spectra are of M dwarfs.
Paper: The Importance of Standardizing Spectra in the Era of Large Spectroscopic Surveys: A Case Study of M Dwarfs in SDSS-V
Authors: Ilija Medan, Zachary Way, Bárbara Rojas-Ayala, Guy S. Stringfellow, Conor Sayres, Keivan G. Stassun, Andrew R. Casey, Sébastien Lépine, Emma Galligan, Diogo Souto, Andrew K. Saydjari
Figure caption: The spectra of the same standard source observed at different MJDs in an RM field. This standard star has 54 epochs of data. It is important to note for the RM fields, that the standard is always observed with the same fiber in the field. Significant changes in the spectral shape are observed. The above spectra were reduced using v6_2_0 of the BOSS pipeline and include data up until MJD = 60715 (2025 February 9).
Paper: The Importance of Standardizing Spectra in the Era of Large Spectroscopic Surveys: A Case Study of M Dwarfs in SDSS-V
Authors: Ilija Medan, Zachary Way, Bárbara Rojas-Ayala, Guy S. Stringfellow, Conor Sayres, Keivan G. Stassun, Andrew R. Casey, Sébastien Lépine, Emma Galligan, Diogo Souto, Andrew K. Saydjari
Figure caption: The first 10 components of the PCA performed on the difference spectra. Here we use reduced BOSS spectra from version v6_1_3 of the pipeline where BP − RP > 1.84, MG > 8.16, π > 2 mas, the SDSS-V program is MWM, SNR > 2, and the target has >3 epochs of observations with a radial velocity measurement. A difference spectrum is then the difference between all combinations of the epoch spectra for the target after they have been radial velocity corrected and normalized with a mean value for 7495 < λ < 7505 Å. The PCA is then performed with a total of 30 components.