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: Plots demonstrating each step in our standardization method as described in Section 3.1.1.
Paper: Increased Molecular Gas Velocity Dispersion and Star Formation Efficiency in Barred Galaxy Centres
Authors: Jennifer M. Laing, Christine D. Wilson
Figure caption: Boxplots comparing the distributions of properties of the central regions for the full sample of barred (42) and unbarred (22) galaxies for each property (top row) and for a subset of the sample containing only galaxies with no AGN, leaving barred (30) and unbarred (19) (bottom row). From left to right, the plots show: area-averaged molecular gas surface density; intensity-weighted molecular gas surface density; intensity-weighted velocity dispersion; SFR surface density; and gas depletion time (both area-averaged). The box encloses the region between the first and third quartiles with the median line shown in orange. Whiskers extend out to 1.5 times the interquartile range and black circles indicate outliers. The gas calculations are done using the linewidth-based αCO from Y.-H. Teng et al. (2024). We find moderate to strong differences between the two full samples for Σmol,IW, σv, ΣSFR, and tdep. However, when galaxies with an AGN are removed from the sample, the only significant differences between the two distributions are found for σv and tdep.
Paper: Increased Molecular Gas Velocity Dispersion and Star Formation Efficiency in Barred Galaxy Centres
Authors: Jennifer M. Laing, Christine D. Wilson
Figure caption: (Left) The Kennicutt–Schmidt relation ΣSFR as a function of Σmol,RA for barred vs. unbarred resolved molecular gas observations of the central region. The two samples agree very well. (Right) σv as a function of ΣSFR for barred vs. unbarred resolved central galaxy properties. Barred galaxies show somewhat increased σv in the central region. Best-fit lines generated with Linmix with slope and intercept uncertainties shown in shaded regions.
Paper: Increased Molecular Gas Velocity Dispersion and Star Formation Efficiency in Barred Galaxy Centres
Authors: Jennifer M. Laing, Christine D. Wilson
Figure caption: Barred vs. unbarred resolved galaxy properties in the central region. (Top) σv as a function of Σmol,IW for the full sample, and (bottom) σv as a function of Σmol,IW for the sample with galaxies with an AGN removed. Best-fit lines generated with Linmix with slope and intercept uncertainties shown in shaded regions. Even once galaxies with an AGN are removed, barred galaxies still show increased σv in the central region.
Paper: Increased Molecular Gas Velocity Dispersion and Star Formation Efficiency in Barred Galaxy Centres
Authors: Jennifer M. Laing, Christine D. Wilson
Figure caption: Boxplots comparing the distributions of the full sample of barred (42) and unbarred (22) galaxies (top row) and sample with no AGN (bottom row) for each property, using the metallicity-dependent αCO. See Figure 1 for description of the quantities and method. The most significant differences between barred and unbarred galaxies for both the full sample and the sample with no AGN, are found for σv and Σmol,IW (see Table B1).
Paper: Increased Molecular Gas Velocity Dispersion and Star Formation Efficiency in Barred Galaxy Centres
Authors: Jennifer M. Laing, Christine D. Wilson
Figure caption: Barred vs. unbarred resolved galaxy properties in the central region using the metallicity-based αCO from J. Sun et al. (2022). ((Top) σv as a function of Σmol,IW for the full sample. (Bottom) σv as a function of Σmol,IW for galaxies without an AGN. Best-fit lines generated with Linmix with slope and intercept uncertainties are shown in shaded regions. Barred galaxies without AGN still show increased σv in the central region.
Paper: An Improved Upper Limit of Cyanodiacetylene (HC5N) in the Atmosphere of Titan
Authors: Takahiro Iino, Kotomi Taniguchi, Hideo Sagawa, Martin A. Cordiner, Shuya Tan, Shigeru Takahashi, Hikaru Kubota
Figure caption: Entire spectral windows corresponding to the J = 96–95 (top) and 99–98 (bottom) transitions of HC5N. Each four and two independent observations were integrated. Blue triangles indicate rest frequencies of HC5N. Known molecular transitions are plotted with markers. ﹩\unicode{9671}﹩, ·, ⋆ and + are for HC3N v6 = 1, HC3N v7 = 2, CH3CCH and C2H3CN. Weak emissions of CH3C3N, reported for the first time in A. E. Thelen et al. (2020), are located at 256.0 GHz region.
Paper: An Improved Upper Limit of Cyanodiacetylene (HC5N) in the Atmosphere of Titan
Authors: Takahiro Iino, Kotomi Taniguchi, Hideo Sagawa, Martin A. Cordiner, Shuya Tan, Shigeru Takahashi, Hikaru Kubota
Figure caption: (Left) Atmospheric temperature profile used for the radiative transfer calculation. (Right) Vertical abundances of HC5N from models of V. Vuitton et al. (2019; black), J. C. Loison et al. (2015; blue), E. Lellouch et al. (2010a; green), and V. A. Krasnopolsky (2009; magenta). Dashed and thick solid profile represent the original abundance profiles from four previous studies and the multiplied 3σ upper limits, respectively.
Paper: An Improved Upper Limit of Cyanodiacetylene (HC5N) in the Atmosphere of Titan
Authors: Takahiro Iino, Kotomi Taniguchi, Hideo Sagawa, Martin A. Cordiner, Shuya Tan, Shigeru Takahashi, Hikaru Kubota
Figure caption: Integrated spectrum using six independent observation of J = 96–95 and 99–98. Blue triangle indicate the rest frequency of HC5N.
Paper: An Improved Upper Limit of Cyanodiacetylene (HC5N) in the Atmosphere of Titan
Authors: Takahiro Iino, Kotomi Taniguchi, Hideo Sagawa, Martin A. Cordiner, Shuya Tan, Shigeru Takahashi, Hikaru Kubota
Figure caption: Integrated spectrum (red) and synthesized spectra (black) produced by four different profiles of E. Lellouch et al. (2010b), J. C. Loison et al. (2015), V. Vuitton et al. (2019), and V. A. Krasnopolsky (2009). Error bars locate at the left side of the panels are 1σ noise level measured at line-free region.
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: AS 209 disk intensity profile in polarized H-band scattered light (solid light blue line, H. Avenhaus et al. 2018) and peak intensity of 12CO (dashed dark blue line, obtained by azimuthally averaging the unobscured east side of the data from S. M. Andrews et al. 2018; V. V. Guzmán et al. 2018 with the GoFish package, R. Teague 2019). Vertical shaded areas report the radial location (1σ uncertainties) of AS 209bkg in the three epochs presented in this paper, while the dashed orange line shows the radial separation of AS 209b (J. Bae et al. 2022). The gray area shows the inner and outer radius of the wide gap observed in the disk (V. V. Guzmán et al. 2018; H. Avenhaus et al. 2018).
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: Corner plot reporting the posterior distribution for the “ISM+Gray” model.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Comparison of ETV data points for all targets derived from light-curve models using allesfitter and from generalized Gaussian fits. Each point represents an individual eclipse event. The red dotted line represents the identity line (y = x), indicating perfect agreement, while the blue dashed line shows the best-fit linear relation, with the equation y = (1.016 ± 0.007)x + (0.066 ± 0.084). The two lines are indistinguishable from each other.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Phase-folded SAP primary-eclipse light curve of TIC 142979644 (black points) with two fitted models overplotted. The allesfitter model (orange) provides a better overall fit, accurately following the steep ingress and egress, as well as the flat mideclipse region. The generalized Gaussian model (blue) is computed using the median values of the fitted parameters; it reproduces the overall eclipse shape but performs less accurately at the sharp ingress/egress transitions and in the mideclipse region, where flux changes occur rapidly.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Mass (either projected or true) vs. orbital periods of the circumbinary (p-type) brown dwarf and planet population derived from NASA Exoplanet Archive, Ö. Baştürk et al. (2023), and E. M. Esmer et al. (2024), including candidates along with (i) all known single host planets, (ii) planets with s-type orbits in multiple-star systems, and (iii) planets of the solar system (green markers).
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: Cluster candidate ages using photometric Paα equivalent widths (see Section 5.2.1 for details). The cyan circles show the distribution of 291 sources with good age estimates using the Starburst99 model (purple). The histograms show the distribution of these sources on each axis with the medians indicated by a vertical line. A majority of our embedded cluster candidates are less than 6 Myr old, with a significant portion less than 5 Myr old (73%). For comparison, six CIGALE models are shown with color indicating the escape fraction modeled. These models show that the age derived will vary significantly at lower equivalent widths and less so for high equivalent widths. The young ages derived via Paα equivalent widths indicate that it is likely that the first supernovae have yet to unbind the natal shroud of gas and dust (S. T. Linden et al. 2023; S. Deshmukh et al. 2024).
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: Number of embedded cluster candidates vs. global star formation properties. Values for each galaxy are in Table 1, and embedded cluster candidate counts from this study are in Table 4. Left: ﹩{{\rm{log}}}_{10}({\rm{SFR}})﹩ vs. number of embedded cluster candidates. Right: ﹩{{\rm{log}}}_{10}({\rm{sSFR}})﹩ vs. number of embedded cluster candidates. The black line in each plot shows the linear fit to the data with the ±1σ region of the fit in light gray. We exclude NGC 2997 and NGC 1097 in fitting due to a lack of wide coverage. The number of embedded cluster candidates positively correlates with each of these properties.
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: An example of an embedded cluster candidate in NGC 3059, denoted by the cyan circle. This source displays point-like emission in F300M and F335M, a significant Pα/Hα excess indicating high levels of extinction, and no visible emission in our HST white-light image. Ideal candidate examples from four galaxies are shown in Appendix A.
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: F335M images of our galaxy sample and the embedded cluster candidates identified in this study. The cyan circles mark the locations of the human-identified embedded cluster candidates in our final catalog. As would be expected for young, dusty clusters, our sample of embedded cluster candidates traces the dusty spiral arms, bars, and rings of their host galaxies. The white, dashed lines indicate the edges of the fields of view for the HST Hα imaging.
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: Histogram of deprojected galactocentric radial distances (rGC) as a fraction of r25 for all 292 embedded cluster candidates. Table 1 gives r25 for each of the galaxies in our sample. The black outline represents the total bin count, and each color denotes the number of clusters from each galaxy.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Similar to Figure 8, but for the UPL group.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Similar to Figure 8, but for the CPL group.
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: Hα index as a function of time in hours, computed using the methodology described in Section 4. The indigo points represent the binned Hα indexes with N = 6 points per bin, while light blue points represent the unbinned Hα indexes. The dashed magenta line shows the transit midpoint and the shaded pink region shows the total transit duration of 1.81 hr. The solid blue line is the Gaussian model that we fit to the data. We measure the increase in Hα index by calculating the amplitude of the Gaussian model, which we find to be δ = 0.00156 ± 0.00026 during the middle of the transit. This is similar in magnitude to the Hα index deviations measured by J. R. Barnes et al. (2016). This signals that the line is becoming shallower while it is occulted by the planet, after normalizing each frame. We interpret this to be a starspot crossing, based on the results of our simulated Hα transit shown in Figures 7 and 8. This deviation is consistent with the planet crossing a starspot with a radius of = 3.47 ± 0.30R⊕. Additionally, we measure the full width half max (FWHM) of the Gaussian model of the Hα indexes to be 0.57 ± 0.13 hr (34 ± 8 minutes), which is comparable to the time it would take for the planet to cross itself, about 24 minutes. This is in line with an occultation of an active region that is smaller than the planet itself, since the planet’s diameter then drives the occultation timescale.
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: Correlation plots of two methods used to check that Hα signal is stellar in origin. Top: Hα index as a function of Fe I index. We measure a Pearson R Correlation Coefficient of ρHα,Fe I = −0.0051 with a p-value of p = 0.95 between Hα index and Fe I index, and ρHα,airmass = −0.067 with a p-value of p = 0.45 between Hα index and air mass. No statistically significant correlation is present, which suggests that the origin of the signal variation we observe in Hα does not appear to strongly impact Fe I. Since this Fe I line is not magnetically sensitive, the origin of this Hα signal could indeed be stellar activity. Bottom: Hα index as a function of air mass of the observation. We again do not see any statistically significant correlation, which suggests that air mass or other observational effects are not the origin of this Hα variation either.
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: SMART image of Hα line center of the solar disk, taken on 2016 July 12 featuring AR 12565. The black box is centered around the active region, and the green box is centered around a quiet region from which flux is pulled for comparison. The image is normalized by the maximum solar flux value. We find Fluxquiet ∼ 0.61 and Fluxspot ∼ 0.37, showing that spots deepen absorption in the Hα line core.
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: Simulated transit of Hα data from Figure 7. The magenta line shows a transit across the actual solar disk, with an impact parameter of 0 to make the transit chord span the most active regions of the solar disk. The blue line shows a transit across a simulated uniform stellar disk that has been limb darkened using a quadratic law, with relevant coefficients of a = 0.2 and b = 0.5 obtained from H. R. Neilson & J. B. Lester (2013).
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: Hα index divided by Fe I index. The blue dots represent the binned index ratio, while the pine green dots represent the unbinned index ratio. The pink shaded region shows the transit duration, and the dashed magenta line shows transit midpoint. This figure shows similar behavior to Figure 3, which indicates that the source of the signal we observe in the Hα index time series is likely not significantly affecting the control Fe I line we observe here. We calculated a Pearson Correlation Coefficient between Hα index and Fe I index and find a coefficient of ρHα,Fe I = −0.0051 with a p-value of p = 0.95, showing there is no statistically significant correlation in Figure 5.
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: Correlation plot of Hα Index versus Index for Telluric Line (λ = 6580.8 Å) selected from the TAPAS Telluric model. This shows the data after removing the 4 outlier points to better illustrate the scatter. We find a Pearson correlation coefficient of ρHα,T = 0.053 with a p-value of p = 0.56 excluding outlier points, which shows there is no statistically significant correlation present.
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: Our analytical solution from Equation (4), along with our measured systemic velocities—obtained by calculating the centers of our simulated observations using the methods outlined in Section 3.1 for Kp values of 80, 158, and 200—are shown. The straight lines represent our analytical solution using Equation (4) and Table 1, while the dotted points represent the measured systemic velocities obtained from our simulated observations. The 1σ error bars indicate the uncertainty in velocity measurements, which were automatically calculated by the code2 used to determine the centers of the CCF matrices. Small offsets in the transit midpoint, on the scale of minutes, result in significant velocity shifts of several km s−1. Moreover, increasing the Kp values amplifies these velocity offsets.
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 planetary radial velocity shifts for different eccentricity offsets for several values of the angle of periastron (ω). The panel on the right plots the radial velocity for different offsets in eccentricity for an original eccentricity value e = 0.12, while the panel on the left does the same for an original eccentricity value of e = 0.05. We can see that small offsets in eccentricity on the order of 0.01 lead to offsets in radial velocities on the order of several km s−1.