adsabs/AstroCLIMB huggingface dataset:
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of HD 192263. This star hosts one giant planet, HD 192263 b. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. The inclination of HD 192263 b is not known, so the line positions show a range from the minimum to maximum possible planetary RVs. Noise from the telluric spectrum is obviously a limiting factor. In future work, the telluric star will be replaced by a synthetic spectrum. The upper limits for H3 + emission for HD 192263 from the Q(1,0) and Q(3,0) lines are 2.3 × 1018 W and 3.2 × 1018 W,, respectively.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of the binary M dwarf–brown dwarf system 2MASS J07200325-084699. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. Expected H3 + line positions are marked by a red vertical dashed line. The upper limits for H3 + emission from the Q(1,0) and Q(3,0) lines are 9.3 × 1016 W and 5.1 × 1016 W, respectively.
Paper: Measuring Elemental Abundances of JWST Target Stars for Exoplanet Characterization. I. FGK Stars
Authors: Jared R. Kolecki, Ji Wang, 吉 王
Figure caption: C/O distribution histograms of this work and various literature sources. The mean values of the distributions are as follows: this work (0.58, LTE with NLTE corrections), Brewer & Fischer (0.48, LTE), Nissen (0.63, LTE with NLTE corrections), Petigura & Marcy (0.76, LTE [O I]).
Paper: Measuring Elemental Abundances of JWST Target Stars for Exoplanet Characterization. I. FGK Stars
Authors: Jared R. Kolecki, Ji Wang, 吉 王
Figure caption: Distribution of C/O ratios of the target stars in LTE and NLTE.
Paper: Implicit Biases in Transit Models Using Stellar Pseudo Density
Authors: Gregory J. Gilbert, Mason G. MacDougall, Erik A. Petigura
Figure caption: Posterior samples of b from a representative selection of DR25 targets before and after reweighting by the Jacobian to correct for biases induced by sampling in ﹩\tilde{\rho }﹩. All targets have 0.02 < r < 0.04 and 10 < P < 30 days. Left panel: raw DR25 posteriors chains show a clear (biased) preference for low values of b. Right panel: after reweighting, the (unbiased) distribution is nearly flat. To minimize spurious peaks and sampling noise in low probability regions, the lowest density 1% of samples have been excluded from our reweighting scheme. The slight increase in probability density near b ≈ 1 in the reweighted posteriors reflects the presence of residual importance sampling noise rather than a real feature of the data. Because there is significant sampling noise (due to the large implied posterior mass in regions with few samples), our preferred method for ameliorating the pseudo-density bias is to refit the photometry.
Paper: Implicit Biases in Transit Models Using Stellar Pseudo Density
Authors: Gregory J. Gilbert, Mason G. MacDougall, Erik A. Petigura
Figure caption: Fractional change in median planet-to-star radius ratio for all planet candidates after correcting posterior chains from DR25 (Thompson et al. 2018) using the Jacobian reweighting scheme described in Section 5. 5σ outliers have been iteratively clipped in order to eliminate spurious values that are expected to arise due to insufficient sampling of low probability regions. There is a spike at δ  r  = 0, indicating that some subset of targets were accurately measured, but the majority of targets are distributed around δ  r /r = 1.6%.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Normalized PDCSAP light curve of TOI-1452 from sectors 15–26 (except 18), 40–41, and 47. Sectors 14 and 21 were previously shown in Figure 2. The blue data points highlight the epochs of the detected transits, while the red data points are outliers/stellar flares rejected by sigma clipping (3.5 σ clip) or manually (in sectors 40, 41, or 47). The gaps in the light curve coincide with data downlink when TESS is close to perigee. The full light curve was modeled with a quasiperiodic Gaussian Process (green curve; details in Section 4.2).
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Mass–radius diagram of exoplanets (gray points). Only planets with mass and radius known with precision better than 30% are shown. Various theoretical composition curves are plotted, using interior structure models from Valencia et al. (2007), Valencia et al. (2013), Guillot & Morel (1995). All models assume no atmosphere, except the H–He (red dashed lines) models that correspond to Earth-like interior surrounded by a solar composition envelope at T = 300 K. The mass and radius posteriors (green 1 and 2σ contours) of TOI-1452b are consistent with either a water-rich interior with ∼25% H2O by mass, a pure rock (rocky threshold radius curve including relevant phase transitions), or a terrestrial planet with a thin hydrogen envelope of ∼0.1% H–He by mass.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Period–radius diagram of exoplanets around low-mass stars (T eff ≤ 4000 K) with mass and radius known with precision better than 30%. The TRAPPIST-1 (T-1) planets are represented by triangles. Empirical valleys for low-mass stars from Cloutier & Menou 2020 (CM20), consistent with gas-depleted formation, and from Martinez et al. 2019 (M19), compatible with thermally driven atmospheric mass loss and scaled down to represent the stellar mass population of CM20. TOI-1452b lies below M19 and has a small bulk density compared to a terrestrial planet of the same mass (ρ/ρ Earth−like ≈ 0.76). This is inconsistent with photoevaporation and core-powered mass-loss predictions.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: TSM (Kempton et al. 2018) as a function of the planetary equilibrium temperature for small exoplanets (R p < 4 R ⊕) with well-established masses (error below 30%). The green region corresponds to an arbitrary temperate temperature interval (200 K ≤ T eq ≤ 400 K). TOI-1452b is among the best temperate targets for follow-up transit spectroscopy with JWST.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Fe/Mg distribution for TOI-1452b according to different model assumptions (Table 9) compared to that of its host star (black). We used kernel density estimate to draw the probabilities from the posteriors. We also include the M dwarfs distribution of Fe/Mg from the APOGEE database (gray histogram, sample size of ∼1000; Majewski et al. 2016; Ahumada et al. 2020) for comparison.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: RV time series from SPIRou and IRD with the best-fit Keplerian + activity GP (orange curve), activity GP-only (red dashed curve), and Keplerian-only (blue curve) models overplotted. The residuals below show an overall agreement between the SPIRou errors and the RV dispersion, which is difficult to assess for IRD given the limited number of measurements.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Phase-folded SPIRou RV curve, with systemic velocity and activity GP removed. Binned RV measurements (0.1 phase bin) are marked with black circles. The best-fit Keplerian models (blue) are depicted with a solid curve (circular orbit) and a dashed curve (eccentric orbit). The residuals of the circular fit are presented below. The circular solution yields smaller residuals rms (3.58 m s−1) compared to the eccentric model (3.66 m s−1); yet both Bayesian evidences are indistinguishable (see Figure 12).
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: No assumptions, corner plot summary for TOI-1452b interior parameters where the core-mass fraction (CMF) and water-mass fraction (WMF) are simulated quantities for a given planetary mass and radius. Chemical ratios Fe/Si and Mg/Si are derived quantities. The vertical red lines in the Fe/Si, Fe/Mg space are the mean stellar refractory ratios, and the vertical dashed lines represent 16th and 84th percentiles.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Stellar prior, corner plot summary for TOI-1452b interior parameters where we assume that the planet follows stellar refractory ratios for a given planetary mass and radius. Thus, the log-probability function is modified to include the restriction posed by the Fe/Mg ratio of the star and can be written as ﹩{\rm{F}}{\rm{e}}/{\rm{M}}{\rm{g}}\sim { \mathcal N }({{\rm{F}}{\rm{e}}}_{\ast }/{{\rm{M}}{\rm{g}}}_{\ast },{{\sigma }}_{{{\rm{F}}{\rm{e}}}_{\ast }/{{\rm{M}}{\rm{g}}}_{\ast }})﹩. The red and dashed vertical lines represent the stellar ratios and 16th and 84th percentiles of the posterior, respectively.
Paper: BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star
Authors: Kyeongsoo Hong, Jae Woo Lee, Pakakaew Rittipruk, Jang-Ho Park, Hye-Young Kim, Cheongho Han
Figure caption: TESS light curve of BD+47 378 with fitted models. In the top panel, the green, yellow, and red lines display the synthetic curves obtained from the unspotted model, Model 1, and Model 2, respectively. As the two spot models are substantially identical, Model 1 is not clearly visible individually. The light residuals from the Model 1 and Model 2 are represented in the middle and bottom panels, respectively.
Paper: BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star
Authors: Kyeongsoo Hong, Jae Woo Lee, Pakakaew Rittipruk, Jang-Ho Park, Hye-Young Kim, Cheongho Han
Figure caption: RV curves of BD+47 378 with fitted models. In the upper panel, the green and pink symbols represent the velocities for the primary and secondary stars, respectively. The lower panel shows the residuals between the measurements and fitted models. The dotted line in the upper panel refers to the system velocity of 4.3 km s−1.
Paper: BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star
Authors: Kyeongsoo Hong, Jae Woo Lee, Pakakaew Rittipruk, Jang-Ho Park, Hye-Young Kim, Cheongho Han
Figure caption: Five spectral regions of the observed spectrum with a phase of 0.504. The red solid line represents the synthetic spectrum of 7140 K with the v 1sini of 32 km s−1.
Paper: BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star
Authors: Kyeongsoo Hong, Jae Woo Lee, Pakakaew Rittipruk, Jang-Ho Park, Hye-Young Kim, Cheongho Han
Figure caption: TESS time-series data of BD+47 378. In the upper panel, the gray circles represent the PDCSAP flux data processed by the SPOC. In the lower panel, the black circles represent the detrended data in magnitude scale.
Paper: BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star
Authors: Kyeongsoo Hong, Jae Woo Lee, Pakakaew Rittipruk, Jang-Ho Park, Hye-Young Kim, Cheongho Han
Figure caption: The 3D models of the Roche geometry and the cool spot regions for the orbital phases of 0.0 and 0.5 based on the binary solutions obtained from Model 2.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Histograms of the number of galaxies as a function of f3 for Yu & Ho (2020) galaxies with z < 0.03 identified by Galaxy Zoo as having one arm (top panel), two arms (second panel), three arms (third panel), four arms (fourth panel), more than 4 arms (fifth panel), or “cannot count arms” (sixth panel). The histograms in black in the top six panels include only “securely identified” spirals that have at least 20 classifications in Galaxy Zoo, and for which at least half of the participants agreed on the number of arms based on vote fractions uncorrected for classification bias. The blue dotted histograms mark the galaxies which were “flagged” by Hart et al. (2016) as having reliable arm counts after correction for classification bias. The bottom panel gives the distribution of f3 for galaxies not considered “secure spirals” in Galaxy Zoo. The black filled diamonds and blue open triangles give the median f3 values for the black and blue histograms, respectively, with the error bars marking the range from the first quartile to the third quartile. The red circle with error bars illustrates the median measurement uncertainty on f3.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Log sSFR vs. log stellar mass for field galaxies (top panel) and galaxies in massive clusters (bottom panel). The sSFRs in these plots come from the GSWLC-2, while the stellar masses on the y-axis come from the NSA. Correlation coefficients for galaxies with 10 ≤ log M* < 11 and log sSFR ≥ −12 are displayed on the corresponding plot. The data points are color coded based on concentration (red: C ≥ 4.5; yellow: 4.0 ≤ C < 4.5; green: 3.5 ≤ C < 4.0; blue: C < 3.5). The galaxies marked by open black squares are classified as AGN (see text for details).
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Plots of f3 vs. the log of the sSFR for field galaxies (top panel) and galaxies in massive clusters (bottom panel). The sSFRs in these plots come from the GSWLC-2. The red line in the bottom plot is the best fit for cluster galaxies with log sSFR ≥ −12 and 10 ≤ log M* < 11. The slope (m), y-intercept (b), and rms of the best-fit lines are printed on the corresponding plot, along with the Spearman (ρ) and Pearson (r) correlation coefficients. The data points are color coded based on concentration (red: C ≥ 4.5; yellow: 4.0 ≤ C < 4.5; green: 3.5 ≤ C < 4.0; blue: C < 3.5). The galaxies marked by open magenta diamonds were classified by Yu & Ho (2020) as either S0-, S0, or SB0.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: The bar strength plotted against the GSWLC-2 sSFR for field galaxies (top panel) and galaxies in massive clusters (bottom panel). In the top panel, the Spearman (ρ) and Pearson (r) correlation coefficients for the field galaxies with log sSFR ≥ −12 and 10 ≤ log M* < 11 are printed. The red line in the bottom panel is the best fit for the log sSFR ≥ −12 and 10 ≤ log M* < 11 galaxies in massive clusters. The slope (m), y-intercept (b), rms, Spearman (ρ), and Pearson (r) correlation coefficients for that line are also provided. The data points are color coded based on concentration (red: C ≥ 4.5; yellow: 4.0 ≤ C < 4.5; green: 3.5 ≤ C < 4.0; blue: C < 3.5).