adsabs/AstroCLIMB huggingface dataset:
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 BOSS spectra from SDSS-V, where each grid point shows the ﹩{\chi }_{\nu }^{2}﹩ between the median spectrum in that bin and all spectra standardized with a given method. In the above, only BOSS spectra within 100 pc, with an SNR > 5 and determined to be true single stars by Z. Way et al. (2025, in preparation) were included in the above. Additionally, only grid points with >5 spectra are shown. All 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 best stellar parameters are found by minimizing the χ2 between the standardized BOSS-like spectra to the standardized BT-NextGen models. This process imitates a typical template matching that would be performed on SDSS-V spectra. The above shows the difference between the true and best-fit parameters vs. the true parameters of the spectrum used to generate the BOSS-like spectra for the various methods. Overall, the scatter is low when the spectra are standardized with our method, and we see very few covariances in the parameters.
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: An example of a set of “BOSS-like” spectra (black lines) generated by adding a random realization of a difference spectrum from our PCA bases, along with some random amount of extinction and noise to a smoothed BT-NextGen model (red line). In this figure, the black lines are 100 random realizations of such a BOSS-like spectrum for a BT-NextGen model with Teff = 3400 K, [Fe/H] = 0 dex, and [α/Fe] = 0 dex. All spectra have been normalized based on the average flux value for 7495 < λ < 7505 Å.
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 best stellar parameters are found by minimizing the χ2 between the standardized BOSS-like spectra to the standardized BT-NextGen models. This imitates a typical template matching that would be performed on SDSS-V spectra. The above shows the difference between the true and best-fit parameters vs. the true parameters of the spectrum used to generate the BOSS-like spectra.
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: Comparison of spectra of 5370 stars in both DESI DR1 and SDSS DR19. The plot shows the running median (solid lines) and 16th and 84th percentiles (shaded region) of the difference in the fluxes relative to the errors. The red is the difference in the reduced, flux-calibrated spectra directly from the pipelines of the respective surveys. The black is the difference in the standardized spectra using our alpha hulling method.
Paper: Direct Measurement of Extinction in a Planet-hosting Gap
Authors: Gabriele Cugno, Stefano Facchini, Felipe Alarcon, Jaehan Bae, Myriam Benisty, Anna-Christina Eilers, Gene C. K. Leung, Michael Meyer, Laurent Pueyo, Richard Teague, Edwin Bergin, Julien Girard, Ravit Helled, Jane Huang, Jarron Leisenring
Figure caption: Astrometry of the AS 209 system. Left: proper motion analysis of AS 209bkg. The red square represents the location of the source in 2005. The black line shows the expected trajectory from 2005 through 2024 assuming it is a stationary object, with the expected locations at the SPHERE and NIRCam epochs highlighted with black circles. The NIRCam and SPHERE data agree with the prediction (when considering the HST uncertainties), demonstrating that the source is indeed a background object. Right: projected location of AS 209bkg in the AS 209 disk. On the right side, the millimeter image is reported, showcasing a series of dust rings (S. M. Andrews et al. 2018). On the left side, the CO gas as measured by the DSHARP program (S. M. Andrews et al. 2018; V. V. Guzmán et al. 2018) is reported. AS 209bkg shines through the deep outer CO gap. Gray crosses mark the expected position of AS 209bkg in 2050 and 2075.
Paper: Direct Measurement of Extinction in a Planet-hosting Gap
Authors: Gabriele Cugno, Stefano Facchini, Felipe Alarcon, Jaehan Bae, Myriam Benisty, Anna-Christina Eilers, Gene C. K. Leung, Michael Meyer, Laurent Pueyo, Richard Teague, Edwin Bergin, Julien Girard, Ravit Helled, Jane Huang, Jarron Leisenring
Figure caption: SED fits for AS 209bkg using multiple extinction models. In each panel, the observed fluxes are reported in blue squares, while detection limits are shown in light blue arrows. The F300M detection limits, potentially impacted by the 3.0 μm water-ice band, is shown for completeness but is not used in the fit. The best-fit model is shown with a black line, while 100 random samples drawn by the posterior distribution are shown in gray. The log-evidence with respect to the “None” scenario (top left) is reported in each panel.
Paper: Direct Measurement of Extinction in a Planet-hosting Gap
Authors: Gabriele Cugno, Stefano Facchini, Felipe Alarcon, Jaehan Bae, Myriam Benisty, Anna-Christina Eilers, Gene C. K. Leung, Michael Meyer, Laurent Pueyo, Richard Teague, Edwin Bergin, Julien Girard, Ravit Helled, Jane Huang, Jarron Leisenring
Figure caption: Same as Figure 7, with the addition of the red square representing the 2005 HST detection, and orange lines that represent the random sample and best-fit model for the 2005 epoch. In this case, the “Gray” model is used to benchmark the Bayesian log-evidences.
Paper: Direct Measurement of Extinction in a Planet-hosting Gap
Authors: Gabriele Cugno, Stefano Facchini, Felipe Alarcon, Jaehan Bae, Myriam Benisty, Anna-Christina Eilers, Gene C. K. Leung, Michael Meyer, Laurent Pueyo, Richard Teague, Edwin Bergin, Julien Girard, Ravit Helled, Jane Huang, Jarron Leisenring
Figure caption: CMD of galactic (orange) and extragalactic (blue) objects, and comparison with AS 209bkg. The object is consistent with the galactic population. The arrows show how AS 209bkg would move on the diagram in the case one would correct for ISM or gray extinction (AV = 2.0 mag for both). When extinction is accounted for, the photometry of AS 209bkg agrees more strongly with the galactic population.
Paper: Direct Measurement of Extinction in a Planet-hosting Gap
Authors: Gabriele Cugno, Stefano Facchini, Felipe Alarcon, Jaehan Bae, Myriam Benisty, Anna-Christina Eilers, Gene C. K. Leung, Michael Meyer, Laurent Pueyo, Richard Teague, Edwin Bergin, Julien Girard, Ravit Helled, Jane Huang, Jarron Leisenring
Figure caption: JWST/NIRCam imaging residuals for F200W and F410M (top row, Cycle 1) and F250M, F323N, and F405N (bottom row, Cycle 3). AS 209bkg (CC 1) is marked by a white arrow. North is pointing up in the image, east to the left. The central mask has a radius of ﹩1\mathop{.}\limits^{^{\prime\prime} }1﹩.
Paper: Direct Measurement of Extinction in a Planet-hosting Gap
Authors: Gabriele Cugno, Stefano Facchini, Felipe Alarcon, Jaehan Bae, Myriam Benisty, Anna-Christina Eilers, Gene C. K. Leung, Michael Meyer, Laurent Pueyo, Richard Teague, Edwin Bergin, Julien Girard, Ravit Helled, Jane Huang, Jarron Leisenring
Figure caption: JWST/NIRCam coronography residuals for F182M, F210M, F300M, and F335M. AS 209bkg (CC 1) is marked by a white arrow, while for the nondetection in F300M the position of the source is marked with a white circle.
Paper: Direct Measurement of Extinction in a Planet-hosting Gap
Authors: Gabriele Cugno, Stefano Facchini, Felipe Alarcon, Jaehan Bae, Myriam Benisty, Anna-Christina Eilers, Gene C. K. Leung, Michael Meyer, Laurent Pueyo, Richard Teague, Edwin Bergin, Julien Girard, Ravit Helled, Jane Huang, Jarron Leisenring
Figure caption: Y- and J-band residuals of AS 209 obtained with VLT/SPHERE. AS 209bkg (CC 1) is marked by a white arrow.
Paper: Direct Measurement of Extinction in a Planet-hosting Gap
Authors: Gabriele Cugno, Stefano Facchini, Felipe Alarcon, Jaehan Bae, Myriam Benisty, Anna-Christina Eilers, Gene C. K. Leung, Michael Meyer, Laurent Pueyo, Richard Teague, Edwin Bergin, Julien Girard, Ravit Helled, Jane Huang, Jarron Leisenring
Figure caption: HST/NICMOS F110W residuals obtained from the ALICE survey (J. B. Hagan et al. 2018). The white arrow points to AS 209bkg (CC 1).
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: F300M – F770W vs. F814W – F335M diagram for consistent Label 1 test objects for models without Paα and F150W data. The black line is the mean empirical template from B. C. Whitmore et al. (2025) for ages of 1–9 Myr (black dots), as this range spans just beyond the timescale we expect for embedded sources (M. J. Rodríguez et al. 2025; L. Ramambason 2025, in preparation; B. C. Whitmore et al. 2025). The reddening vector (maroon) is for AV = 6, representative of the median we derive in Section 5.2.2 for our by-eye sample.
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: Left: normalized histogram of 181 of our embedded cluster candidates (ECC, cyan), 1117 AGB stars (AGB, pink), and 2308 HST Class 1+2 optical clusters (OC, orange; D. Maschmann et al. 2024) with F150W concentration index CIF150W greater than zero and a peak S/N > 5. Bins are normalized to the total number of objects and the bin width. The solid vertical lines indicate the median for each distribution of objects. The bimodal distribution of the embedded cluster candidates may be indicative of evolved stars present within our by-eye sample. Right: F150W surface brightness against CIF150W, where color indicates the age derived via Paα equivalent-width age dating. The scatter shows our embedded cluster candidates, and the contours denote the 10th,  50th,  and 90th percentiles of HST Class 1+2 optical clusters for 3–5 Myr (dark purple) and greater than 5 Myr (light purple). The dashed vertical line at CI = 1.4 marks the limit B. C. Whitmore et al. (2023) uses to distinguish between stars and clusters in the JWST F200W band. The median CIF150W is 1.22 for embedded cluster candidates with ages greater than 5 Myr and 1.69 for sources in the 3–5 Myr age bin.
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: Confusion matrices for all eight model configurations, normalized to the number of objects tested in each “True Label” category (see Table 3 for the number of objects in each class). The numbers below the percentages are the average and standard deviation of the model agreement in each quadrant. Left: confusion matrices for models that include F150W and Paα data in training. Right: confusion matrices for models which exclude F150W and Paα data in training.
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: 3.3 μm/3.0 μm flux ratio vs. stellar population age for our embedded cluster candidate sample (cyan circles) and the HST Class 1+2 optical clusters from D. Maschmann et al. (2024) for five galaxies in our sample (orange diamonds). The vertical orange lines denote the 10th to 90th percentile range for each age bin, and the diamond marks the 50th percentile for the Class 1+2 clusters. Optical cluster ages are from D. Thilker et al. (2024), and embedded cluster candidate ages are from Section 5.2.1 of this work. We compare these values to the empirical template from B. C. Whitmore et al. (2025), reddened for an AV = 6 (black track).
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: Paα flux vs. F335M/F300M flux ratio for Label 1 objects in Figure 9 (left). The dashed lines indicate the median along each axis for the training samples: Label 0 (black) and Label 1 (orange).
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: A histogram of the distribution of masses for the subset of 186 embedded cluster candidates with an F150W peak pixel S/N > 5. There are two sources with mass estimates below 102 M⊙ not shown. The maroon error bars show the 1σ standard deviations from Monte Carlo simulations for each bin with at least one embedded cluster candidate.
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: Example ideal cluster candidates as seen in the Zooniverse interface (left), a three-color NIRCam image (center), and a three-color HST image (right). From top to bottom, we show one candidate from NGC 1097, NGC 1559, NGC 2775, and NGC 2997. The four cutouts in the left panel are 2﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 cutouts centered on the source using the same images as Figure 2, with the cyan circle denoting the final F335M source center. The three-color images also display a 2﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 cutout centered on the source. The individual bands are shown in the small boxes above the composite image.
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: Scatter of [N II]/Hα vs. ﹩{{\rm{log}}}_{10}({M}_{* })﹩. We select 17 galaxies at a distance of less than 11 Mpc which have ﹩{{\rm{log}}}_{10}({M}_{* })﹩ values available from A. K. Leroy et al. (2021), as well as [N II]/Hα estimates from R. C. Kennicutt et al. (2008; cyan circles). The linear fit (black line) to these data is used to determine [N II]/Hα for the 11 galaxies studied in this work (magenta diamonds).
Paper: PAH Marks the Spot: Digging for Buried Clusters in Nearby Star-forming Galaxies
Authors: Gabrielle B. Graham, Daniel A. Dale, Chase L. Smith, Elisabeth Brann, Kaycee D. Conder, Samuel Crowe, Sumitra Dhileepkumar, Nicole A. Imming, Emilio Mendez, Zachary Pleska, Kelsey Sako, Amirnezam Amiri, Ashley T. Barnes, Médéric Boquien, Rupali Chandar, Ryan Chown, Oleg Y. Gnedin, Kathryn Grasha, Stephen Hannon, Hamid Hassani, Rémy Indebetouw, Hwihyun Kim, Jaeyeon Kim, Hannah Koziol, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Elias K. Oakes, M. Jimena Rodríguez, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Leonardo Ubeda, Bradley C. Whitmore, Tony D. Weinbeck, Thomas G. Williams, Aida Wofford, J. Eduardo Méndez-Delgado, Qiushi Chris Tian
Figure caption: Distribution of AV for the 291 visually identified embedded cluster candidates with good age estimates. A large portion (∼98%) of our embedded cluster candidates exhibit AV values greater than 3 mag, which most likely is a reflection of our by-eye selection criteria.
Paper: An Hα Transit of HD 189733b to Assess Stellar Activity Across the Transit Chord Close to JWST Observations
Authors: Kingsley E. Ehrich, Jason A. Dittmann, Samuel P. Halverson, Alejandro Camazón-Pinilla
Figure caption: Example R ∼ 20,000 MEGARA spectrum of HD 189733 after extraction and normalization, with the TAPAS telluric model (J. L. Bertaux et al. 2014) overlaid in the Earth rest frame. The solid blue line is the MEGARA spectra of HD 189733, and the solid red line is the TAPAS telluric model. The teal dot represents the telluric peak in the MEGARA data, while the violet dot represents the telluric peak in the TAPAS telluric model. Both have a wavelength of λ = 6580.8 Å in the Earth rest frame. We also have labeled the Hα spectral line in magenta and the Fe I reference line in blue. The Fe I reference line is chosen due to its proximity to Hα and its low Landé g factor of geff = 0.820, which was retrieved from the Vienna Atomic Line Database 3 (VALD).
Paper: An Hα Transit of HD 189733b to Assess Stellar Activity Across the Transit Chord Close to JWST Observations
Authors: Kingsley E. Ehrich, Jason A. Dittmann, Samuel P. Halverson, Alejandro Camazón-Pinilla
Figure caption: MEGARA spectrum of Hα within its feature window of 6557.9–6567.6 Å. The larger magenta dots represent the original spectral data points, while the smaller blue dots represent the interpolated data points used to integrate along 0.4 Å window about the line center (see Section 4). The solid orange lines denote this integration window, and the dashed orange line denotes the line center.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: A schematic illustration of the NGVS morphological classification scheme for a selection of high-mass (M* ≥ 109M⊙) galaxies. The six possible structural codes are arranged roughly from early to late types (E → S → I), including “transitional” categories (ES, SI, EI). The three rows correspond to the three possible star formation codes: Quiescent (Q), Intermediate (I), and Active (A). Galaxies are labeled by their NGVS identification number—or VCC number if the galaxy was previously cataloged in the VCC (B. Binggeli et al. 1985)—morphology and stellar mass. Empty entries in this matrix, denoted by an “X,” are either galaxies that do not exist in nature or plausibly exist but are not found in the NGVS, as explained in the text.