adsabs/AstroCLIMB huggingface dataset:
Paper: Resonant and Ultra-short-period Planet Systems Are at Opposite Ends of the Exoplanet Age Distribution
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Jacob H. Hamer
Figure caption: Stellar velocity dispersion as a function of age for the Kepler field. The age–velocity dispersion relation is the same as in Figure 1. We plot as horizontal lines the velocity dispersions of the Hamer & Schlaufman (2020) sample of Kepler-discovered hot Jupiter systems as well as our sample of USP planet systems. We define proto-USP planets as confirmed planets from the Kepler cumulative planet catalog with planet radii R p < 2 R ⊕ and orbital periods 1 day < P < 2 days, and we plot as the dark green horizontal line that sample’s velocity dispersion. Our USP planet system sample has a characteristic mean age 4.7 Gyr ≲ τ ≲ 5.8 Gyr, while the proto-USP planet sample has a characteristic mean age 4.1 Gyr ≲ τ ≲ 4.3 Gyr. We argue that the best explanation for this age offset is that USP planets tidally migrated from longer-period orbits due to cycles of secular eccentricity excitation and tidal damping in multiple-planet systems.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: One-dimensional normalized KDEs of the planet radius distribution for the ρ ≤ 100 (top left), ρ > 300 (top right), and full samples (bottom row), shown in purple, and the Berger et al. (2020) single star sample, shown in black. The radius regime where a given planetary radius could be detected by fewer than 90% of the systems is shaded gray. The thin lines behind each KDE are random draws from each sample, with the binary planets randomly perturbed based on their error and the Berger et al. (2020) sample redrawn with the same sample size as the binaries. The small-separation sample shows a smaller relative number of sub-Neptunes, while the wider-separation sample resembles the Berger et al. (2020) single star distribution with a possible shift in the location of the radius gap.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: KDEs of 100 random draws from the planet radius posteriors from the ≤100 au sample, with each draw composed of a 50/50 mixture of primary and secondary star hosts (in green), compared to the Berger et al. (2020) radius distribution in black. Although the addition of secondary star hosts increases the spread and occasionally leads to a planet radius peak at larger radii, the overall structure of the KDE is not impacted by the inclusion of planets around the secondaries.
Paper: Revising Properties of Planet–Host Binary Systems. IV. The Radius Distribution of Small Planets in Binary Star Systems Is Dependent on Stellar Separation 
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Trent J. Dupuy, Elise Evans, Eric Gaidos, Daniel Huber, Michael J. Ireland, Andrew W. Mann, Erik A. Petigura, Pa Chia Thao, Mackenna L. Wood, Jingwen Zhang
Figure caption: Same as Figure 7 for the ≤100 au sample, except with the primary star radius assumed to be the stellar radius from Berger et al. (2018) or Mathur et al. (2017), instead of the result from our reanalysis using a 1 Gyr isochrone prior on the ages. The result does not change significantly between the two different stellar radius assumptions, as discussed in the text.
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: Low-resolution optical spectra of the Haro 5-2A and B components, as obtained on UT 2021-11-19 with the GHTS instrument at SOAR. In the upper panels, the M2.5 WTTS Haro 5-2A component has Hα weakly in emission. In the lower panels, the accreting M3 CTTS Haro 5-2B component has a strong Hα emission line and the entire Balmer series is in emission. Lithium is moderately strong. Ca H and K are also found strongly in emission, as well as the He I lines. Finally, the Ca II near-IR triplet is in emission.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: Equivalent width of Hα (plotted as ﹩{\mathrm{log}}_{10}(10-{W}({\rm{H}}\alpha )﹩) as a function of spectral type for Haro 5-2A and B, at each epoch for which we obtained low-resolution spectra at SOAR. Haro 5-2A is plotted as large purple boxes, and Haro 5-2B as large red boxes. For comparison, the Orion TTSs from Briceño et al. (2019) are also shown: CTTSs as red circles, and WTTSs as smaller blue dots. The separation between CTTS and WTTS as defined by White & Basri (2003) is shown with the black dashed line, while the criterion adopted by Barrado et al. (2011) is plotted as a dashed–dotted magenta line. The transition region adopted by Briceño et al. (2019) between CTTS and WTTS is shown by the pale green region where C/W objects fall (shown as green dots).
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: High-resolution spectra of the Hα line of the Haro 5-2A and B components, obtained with the SOAR GHTS on UT 2021-11-19. Upper panel: spectrum of the M2.5 WTTS Haro 5-2A. Lower panel: spectrum of the accreting M3-type CTTS Haro 5-2B. The vertical dashed line is set at the rest wavelength for Hα (6562.8 Å). The blue horizontal dashed line indicates the full width of the Hα profile at 10% of its full height (White & Basri 2003).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: Top: Haro 5-2 is located in a little studied part of Orion, west of σ Ori and south of ϵ Ori, both of which are associated with groups of low-mass young stars. Image from ESASky. Bottom: near-IR JHK color composite of Haro 5-2 obtained with adaptive optics on the Gemini-North telescope. The small blue halos are due to a slight elongation of the J image.
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: Left: spectral energy distribution from SIMBAD of the integrated light from the Haro 5-2 quadruple with data from SkyMapper, the Sloan Digital Sky Survey, PanSTARRS, Johnson, the Two Micron All Sky Survey, AKARI, and WISE. Right: WISE images with Haro 5-2, 5-3, and 5-4 marked. The field is about 0.84 pc wide at the distance of Haro 5-2.
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: Equivalent width of Hα as a function of the 10% width of the Hα line profile, for Haro 5-2A (large blue boxes) and Haro 5-2B (large red boxes), measured in the two epochs during which we obtained high-resolution spectra at SOAR. Data are also shown for the Orion TTS from Briceño et al. (2019): CTTSs as red dots, WTTSs as smaller cyan dots, and C/Ws as green diamonds. The separation between CTTSs and WTTSs as defined by White & Basri (2003) is shown with the vertical blue dashed line at 270 km s−1.
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption:  H-band spectra of the individual Ba and Bb components resolved with adaptive optics and GNIRS at the Gemini-North 8 m telescope. Wavelength is in microns and flux is in Wm−2 μm−1.(The data used to create this figure are available in the online article.The data used to create this figure are available.)
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: Near-IR spectra of Haro 5-2A and Haro 5-2B obtained with TSpec at the SOAR telescope. Note the Paβ and Brγ emission lines in Haro 5-2B. Wavelength intervals with strong terrestrial opacity are excluded.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
Authors: Bo Reipurth, C. Briceño, T. R. Geballe, C. Baranec, S. Mikkola, A. M. Cody, M. S. Connelley, C. Flores, B. A. Skiff, J. D. Armstrong, N. M. Law, R. Riddle
Figure caption: TESS light curves of the combined light from the four components of Haro 5-2 from around 2018 December (Sector 6; top) and around 2020 December (Sector 32; bottom). For Sector 6, the cadence was once every 30 minutes, and for Sector 32, it was once every 10 minutes.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The results of cross-correlating our red-arm observations with an atmospheric Fe model (see Figure 5). Top: the 2D K  p –RV map, with the location of the peak correlation signal indicated by white dashed lines. The color bar indicates the significance of the map, as determined by dividing out the standard deviation of regions away from the peak signal (see Section 4.3). A clear correlation signal is visible near the expected planetary location. Bottom: a slice of the 2D K  p –RV map at K  p  = 201 km s−1 (i.e., the K  p  at the peak correlation signal). The dashed black line indicates the location of the signal peak, and the SNR is the same as that indicated by the color bar.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The results of applying the SYSREM algorithm to the first 11 orders (top three rows) and last 11 orders (bottom three rows) in the blue arm of the spectrograph. Top row: the data reduced by DRAGONS. Note that there may be some overlap in wavelength between subsequent orders; each order is displayed separately. Middle row: the results of applying eight iterations of SYSREM to the data. At this point, the telluric and stellar absorption features have been removed, and the planetary signal is buried in the noise. Bottom row: the standard deviation of the data after applying SYSREM. The y-scale is the same for all plots in this row.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The combined blue and red 2D K  p –RV maps for the species which were not detected in this work. The plots are as described in the caption of Figure 7, and the species are indicated in the bottom-right corners. The expected location of the planetary signal (i.e., RV = 0 km s−1, K  p  ∼ 197 km s−1) is marked in dashed white lines. The color bar indicates the SNR as calculated via the standard deviation map.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The results of our model injection/recovery tests, as described in Section 5.3. The plots are as described in the caption of Figure 8, though we note that the injected signal is expected to be present at −K  p  rather than K  p  (as indicated by the white dashed lines).
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The same as Figure 10, but for the first 11 orders (top three rows) and next 11 orders (bottom three rows) in the red arm of the spectrograph. As explained in Section 3.2, we applied six iterations of SYSREM to the red data.
Paper: High-resolution Dayside Spectroscopy of WASP-189 b: Detection of Iron during the GHOST/Gemini South System Verification Run
Authors: Emily K. Deibert, Adam B. Langeveld, Mitchell E. Young, Laura Flagg, Jake D. Turner, Peter C. B. Smith, Ernst J. W. de Mooij, Ray Jayawardhana, Kristin Chiboucas, Roberto Gamen, Christian R. Hayes, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Vinicius M. Placco, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, David O. Jones, Kathleen Labrie, Susan Ridgway, Joanna Thomas-Osip
Figure caption: The same as Figure 11, but for the last eight orders in the red.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Left panel shows the difference between observed W1 (resp. W2 on the y-axis) and the predicted ﹩\widehat{W}1﹩ (resp. ﹩\widehat{W}2﹩). We select stars with a high error in both bands as a preliminary sample of IR-excess candidates, depicted in red (cuts are shown as dashed gray lines, corresponding to Equation (8)). The right panel shows the mean across seven folds of the prediction error, divided by the median absolute error of the object’s 30 nearest neighbors in the respective fold. Error bars are standard deviations across the seven folds. We select another set of candidates in this space, depicted in orange. Red data points match the ones in the left panel, and respectively the orange points match the ones in the right panel.
Paper: The K2 and TESS Synergy. III. Search and Rescue of the Lost Ephemeris for K2's First Planet
Authors: Erica Thygesen, Joseph E. Rodriguez, Zoë L. de Beurs, Andrew Vanderburg, John H. Livingston, Jonathon Irwin, Alexander Venner, Michael Cretignier, Karen A. Collins, Allyson Bieryla, David Charbonneau, Ian J. M. Crossfield, Xavier Dumusque, John Kielkopf, David W. Latham, Michael Werner
Figure caption: Time series and periodograms of the CALM-predicted stellar variability. In the left panels, the DRS pipeline radial velocities and the stellar variability predictions from CCF indices 1, 2, 3, 4, and 5 are plotted as a function of time. The location of these CCF indexes are indicated in Figure 3. On the right panel, the Lomb–Scargle periodograms of the corresponding RV time series are plotted. In yellow, the Keplerian period of K2-2 is indicated in the periodograms. We do not see signals at this planetary period, which provides reassurance that CALM is not absorbing or creating planetary signals.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Left panel shows our initial sample of 18 million FGK-type stars in Gaia DR3 with good crossmatches in AllWISE and 2MASS, in the color–absolute magnitude space. The absolute magnitudes were computed as shown in Equation (3), and there were no corrections made for extinction or reddening by dust here. We plot IR-excess candidates from the literature that appear in this preliminary sample: from Cotten & Song (2016, cyan, targeting nearby stars), Cruz-Saenz de Miera et al. (2014, pink, targeting Sun-like stars), and Moór et al. (2021, blue, targeting EDDs). Our final prime set of candidates is shown in red. The dashed black box illustrates our main-sequence cut. Right panel shows the final sample used for our search, after our main-sequence cut, dust cut, and unWISE control cut as described in Section 2.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Histograms of distribution of our candidates’ sample (dark red outline) and our full 4.9 million star sample (blue) in B  p  − R  p , effective temperature, [M/H], and M  G .
Paper: The K2 and TESS Synergy. III. Search and Rescue of the Lost Ephemeris for K2's First Planet
Authors: Erica Thygesen, Joseph E. Rodriguez, Zoë L. de Beurs, Andrew Vanderburg, John H. Livingston, Jonathon Irwin, Alexander Venner, Michael Cretignier, Karen A. Collins, Allyson Bieryla, David Charbonneau, Ian J. M. Crossfield, Xavier Dumusque, John Kielkopf, David W. Latham, Michael Werner
Figure caption: Projected difference in the time of transit for K2-2 b to the year 2030 using the original ephemeris (gray) and the new ephemeris from this work (purple). Shaded regions indicating up to the 3σ level uncertainty are shown. The inset shows the updated ephemeris, zoomed in for clarity.
Paper: The K2 and TESS Synergy. III. Search and Rescue of the Lost Ephemeris for K2's First Planet
Authors: Erica Thygesen, Joseph E. Rodriguez, Zoë L. de Beurs, Andrew Vanderburg, John H. Livingston, Jonathon Irwin, Alexander Venner, Michael Cretignier, Karen A. Collins, Allyson Bieryla, David Charbonneau, Ian J. M. Crossfield, Xavier Dumusque, John Kielkopf, David W. Latham, Michael Werner
Figure caption: Mass–radius diagram for K2 sub-Neptunes (R  P  = 2.0−3.0 R ⊕). The large black circle is K2-2 b, while the small gray circles are other sub-Neptunes with measured masses from the NASA Exoplanet Archive. The lines represent composition tracks from Zeng et al. (2016).
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Distribution of our full sample and our candidates in Galactic coordinates. Dashed black lines indicate abs(b) = 10.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: Feature Importance from two RFs fitted to predict W1 (blue) and W2 (red).
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: SED and blackbody fitting for our excess candidates. Yellow triangles are the observations gathered and used by Ariadne to compute the SED (dashed dark red line). Red points are the unWISE (for W1 and W2) and AllWISE (for W3 and W4) values. Blue points are the prediction of our model. The best-fit blackbody is depicted as a gray dashed line. The final SED computed as Ariadne SED + blackbody is depicted as a solid black line. Each plot also displays imaging from AllWISE (W1 and W2) and DSS of a ﹩3^{\prime} ﹩ square centered on the source candidate. The bottom part of each plot is the XP absolute spectra from Gaia DR3 computed using Gaiaxpy of the object (in red). The spectra of the 30 nearest neighbors (using NN-mag) are given in gray. The Hα line is shown in blue. The letters above W3 and W4 are AllWISE photometric quality flags.
Paper: A Data-driven Search For Mid-infrared Excesses Among Five Million Main-sequence FGK Stars
Authors: Gabriella Contardo, David W. Hogg
Figure caption: SED, imaging, and XP spectra of IR-deficit candidates.
Paper: The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-floating Planets
Authors: Adam B. Langeveld, Aleks Scholz, Koraljka Mužić, Ray Jayawardhana, Daniel Capela, Loïc Albert, René Doyon, Laura Flagg, Matthew de Furio, Doug Johnstone, David Lafrèniere, Michael Meyer
Figure caption: Results of the spectroscopic survey for object NIRISS-NGC1333-1 (NN1). Top panel: NIRISS WFSS spectrum (dark blue) with flux scaled to a value of 1 at a wavelength of 1.4 μm, and best-fit template (salmon pink) from Section 4.2 that has been smoothed using a Savitzky–Golay filter. Middle-left panels: NIRISS images of the object in the F150W and F200W filters with a 1″ scale. Bottom-left panels: calibrated slope image cutouts that are produced by the calwebb_spec3 pipeline for the NIRISS F150W and F200W filters and modified to apply the background subtraction. Bottom-right panel: map of the metric calculated as part of the spectral fitting. The templates that most closely fit the data (having lowest M; see Equation (1)) are located in the darkest regions. The best solution is marked with a yellow box, and the corresponding template is displayed in the top panel to compare to the observed spectrum. The remaining best nine solutions are marked in orange.